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{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "Blackbody Radiation",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The curves of emitted radiation from blackbodies of different temperatures. The x-axis shows wavelength and the y-axis shows the amount of energy emitted every second by a square meter of the surface of that blackbody at each wavelength.\r\n\r\nThe hotter the body, the shorter the wavelength and the bluer the light it emits its maximum amount of energy at. Despite the coolest body in this plot peaking in red light, the other hotter bodies all emit more red light than the coolest body.",
"alt_text": "Three curves with radiation on the y-axis & wavelength on the x-axis. The cooler curves have redder & lower peaks",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_en_Me9RD4R.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_en_YLoUGRR.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "Blackbody Radiation - UV Catastrophe",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The curves of emitted radiation from blackbodies of different temperatures. The x-axis shows wavelength and the y-axis shows the amount of energy emitted every second by a square meter of the surface of that blackbody at each wavelength.\r\n\r\nThe hotter the body, the shorter the wavelength and the bluer the light it emits its maximum amount of energy at. Despite the coolest body in this plot peaking in red light, the other hotter bodies all emit more red light than the coolest body. \r\n\r\nThe dotted line shows the emitted radiation predicted by classical theory prior to modern quantum mechanics. This prediction tends to infinity at shorter wavelengths for any blackbody temperature above zero and was dubbed the ‘ultraviolet catastrophe’.",
"alt_text": "Three curves with radiation on the y-axis & wavelength on the x-axis. The cooler curves have redder & lower peaks",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_en_IfcZd6D.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_en_14NqjQI.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "Schwarzkörperstrahlung - UV-Katastrophe",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Die Kurven der emittierten Strahlung von Schwarzen Körpern unterschiedlicher Temperatur. Die x-Achse zeigt die Wellenlänge und die y-Achse die Energiemenge, die pro Sekunde von einem Quadratmeter der Oberfläche dieses Schwarzen Körpers bei jeder Wellenlänge abgegeben wird. Je heißer der Körper ist, desto kürzer ist die Wellenlänge und desto blauer ist das Licht, bei dem er seine maximale Energiemenge abgibt. Obwohl der kühlste Körper in diesem Diagramm ein Maximum im roten Licht aufweist, strahlen die anderen heißeren Körper alle mehr rotes Licht ab als der kälteste Körper. Die gepunktete Linie zeigt die Strahlung, die von der klassischen Theorie vor der modernen Quantenmechanik vorhergesagt wurde. Diese Vorhersage tendiert bei kürzeren Wellenlängen für jede Schwarzkörpertemperatur über Null gegen unendlich und wurde als \"Ultraviolettkatastrophe\" bezeichnet.",
"alt_text": "Strahlungsmenge als Funktion der Wellenlänge mit drei Kurven. Die kühleren Kurven haben rötere und niedrigere Maxima",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "de",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_de.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_de.pdf",
"diagram_url": "https://astro4edu.org/de/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "Schwarzkörperstrahlung",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Die Kurven der emittierten Strahlung von Schwarzen Körpern unterschiedlicher Temperatur. Die x-Achse zeigt die Wellenlänge und die y-Achse die Energiemenge, die pro Sekunde von einem Quadratmeter der Oberfläche dieses Schwarzen Körpers bei jeder Wellenlänge abgegeben wird. Je heißer der Körper ist, desto kürzer ist die Wellenlänge und desto blauer ist das Licht, bei dem er seine maximale Energiemenge abgibt. Obwohl der kühlste Körper in diesem Diagramm ein Maximum im roten Licht aufweist, strahlen die anderen heißeren Körper alle mehr rotes Licht ab als der kühlste Körper.",
"alt_text": "Strahlungsmenge als Funktion der Wellenlänge mit drei Kurven. Die kühleren Kurven haben rötere und niedrigere Maxima",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "de",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_de.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_de.pdf",
"diagram_url": "https://astro4edu.org/de/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "Radiação de corpo negro",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "As curvas da radiação emitida por corpos negros de diferentes temperaturas. O eixo x mostra o comprimento de onda e o eixo y mostra a quantidade de energia emitida a cada segundo por um metro quadrado da superfície desse corpo negro em cada comprimento de onda.\r\n\r\nQuanto mais quente o corpo, menor o comprimento de onda e mais azul a luz em que ele emite sua quantidade máxima de energia. Apesar de o corpo mais frio nesse gráfico ter um pico de luz vermelha, todos os outros corpos mais quentes emitem mais luz vermelha do que o corpo mais frio.",
"alt_text": "Curvas com radiação no eixo y e comprimento de onda no eixo x. As curvas mais frias têm picos mais vermelhos e mais baixos",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "pt-br",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_pt-br.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_pt-br.pdf",
"diagram_url": "https://astro4edu.org/pt-br/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "Radiação de corpo negro - Catástrofe do UV",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "As curvas da radiação emitida por corpos negros de diferentes temperaturas. O eixo x mostra o comprimento de onda e o eixo y mostra a quantidade de energia emitida a cada segundo por um metro quadrado da superfície desse corpo negro em cada comprimento de onda.\r\n\r\nQuanto mais quente o corpo, menor o comprimento de onda e mais azul a luz em que ele emite sua quantidade máxima de energia. Apesar de o corpo mais frio nesse gráfico ter um pico de luz vermelha, todos os outros corpos mais quentes emitem mais luz vermelha do que o corpo mais frio.\r\n\r\nA linha pontilhada mostra a radiação emitida prevista pela teoria clássica antes da mecânica quântica moderna. Essa previsão tende ao infinito em comprimentos de onda mais curtos para qualquer temperatura de corpo negro acima de zero e foi chamada de \"catástrofe do ultravioleta\".",
"alt_text": "Curvas com radiação no eixo y e comprimento de onda no eixo x. As curvas mais frias têm picos mais vermelhos e mais baixos",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "pt-br",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_pt-br.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_pt-br.pdf",
"diagram_url": "https://astro4edu.org/pt-br/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Spectrum of an O-type star",
"diagram_slug": "m5801x5SA50",
"diagram_title": "Spectrum of an O-type star",
"glossary_terms": [
328,
382,
463
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectrum of the O-type star HD 235673 with wavelength in nanometers on the x-axis and flux on the y-axis. The top part of the plot shows the same spectrum but with bright patches for wavelengths with high flux and dark patches for wavelengths with low flux. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. For O-type stars the most important features are a small number of lines caused by ionized helium. These lines are stronger in O-type stars than in cooler stars. Lines from helium atoms and hydrogen atoms also appear in the spectrum. The spectrum has more flux at the blue end of the spectrum than at the red end of the spectrum.",
"alt_text": "A smooth line declining at longer wavelengths with a few sharp dips.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-o-type-star_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-o-type-star_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/m5801x5SA50/"
},
{
"diagram_label": "Spectrum of a B-type star",
"diagram_slug": "QF74Q764Tb95",
"diagram_title": "Spectrum of a B-type star",
"glossary_terms": [
37,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectrum of the B-type star HD 258982. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. For B-type stars the most important lines are caused by helium atoms. These lines are strongest in B-type stars and weaker in hotter and cooler types. Lines from hydrogen atoms are also present but are not as strong as in cooler A-type stars.",
"alt_text": "A smooth line declining at longer wavelengths with a few sharp dips.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-b-type-star_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-b-type-star_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/QF74Q764Tb95/"
},
{
"diagram_label": "Spectrum of an A-type star",
"diagram_slug": "2149RS77wy92",
"diagram_title": "Spectrum of an A-type star",
"glossary_terms": [
1,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectrum of the A-type star BD-11 1212. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. Lines from hydrogen atoms dominate the spectra of A-type stars and are strongest at this spectral type.",
"alt_text": "A smooth line peaking about 420 nm then declining at longer wavelengths with a few fairly broad dips.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-a-type-star_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-a-type-star_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/2149RS77wy92/"
},
{
"diagram_label": "Spectrum of an F-type star",
"diagram_slug": "zY580V14PE47",
"diagram_title": "Spectrum of an F-type star",
"glossary_terms": [
110,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectrum of the F-type star 2MASS J22243289+4937443. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. The lines from hydrogen atoms that are strongest in A-type stars are still relatively strong in F-type stars but lines from metals, particularly ionised calcium begin to become strong at this spectral type.",
"alt_text": "A relatively smooth line peaking about 430 nm then declining at longer wavelengths with a few fairly broad dips.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-f-type-star_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-f-type-star_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/zY580V14PE47/"
},
{
"diagram_label": "Spectrum of a G-type star",
"diagram_slug": "mX21es50Pj16",
"diagram_title": "Spectrum of a G-type star",
"glossary_terms": [
328,
382,
442
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectrum of the G-type star UCAC4 700-069569. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. In G-type stars lines from hydrogen atoms are weaker than in F-type stars and lines from ionised calcium stronger. Lines from metal atoms such as atoms of iron, sodium and calcium also begin to become prominent.",
"alt_text": "A quite ragged line peaking about 470 nm then declining at longer wavelengths with a few deeper dips.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-g-type-star_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-g-type-star_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/mX21es50Pj16/"
},
{
"diagram_label": "Spectrum of a K-type star",
"diagram_slug": "lH42QC364e69",
"diagram_title": "Spectrum of a K-type star",
"glossary_terms": [
168,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectrum of the K-type star 2MASS J19554455+4754531. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. The spectra of K-type stars are dominated by metal atoms such as iron, sodium and calcium atoms. There are so many lines from metal atoms, far too many to mark individually, that the spectrum has a choppy, ragged appearance. The lines of hydrogen atoms and calcium ions are much weaker than in the hotter G-type stars.",
"alt_text": "A ragged line peaking about 580 nm then declining at longer wavelengths with a few deeper dips.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-k-type-star_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-k-type-star_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/lH42QC364e69/"
},
{
"diagram_label": "Spectrum of an M-type star",
"diagram_slug": "d156Ob46Ih98",
"diagram_title": "Spectrum of an M-type star",
"glossary_terms": [
328,
382,
453
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectrum of the M-type star 2MASS J15581272+8457104. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe black lines show spectral absorption lines caused by atoms, ions and molecules of different elements in the star’s atmosphere. These atoms, ions and molecules absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. The atmospheres of M-type stars are cool enough for some chemical compounds to form. These are often referred to as molecules in astronomy, even if they are not strictly molecules in chemistry. These molecules produce so many lines in an M-type star’s spectrum that the lines appear to merge together in huge bands that remove large chunks from the spectrum. In M-type stars, titanium oxide has a large number of these bands in visible light, dominating huge regions of the spectrum.",
"alt_text": "A choppy line increasing at longer wavelengths with large wide dips and a few sharper dips.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-m-type-star_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-m-type-star_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/d156Ob46Ih98/"
},
{
"diagram_label": "Stellar spectral types",
"diagram_slug": "Tt35DR10iI63",
"diagram_title": "Stellar spectral types",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectra of seven stars ordered by spectral type ranging from the hottest (O-type) at the top to the coolest (M-type at the bottom). The x-axis shows the wavelength of light and the y-axis is a measure of the flux of light received at that wavelength. Each spectrum is normalized (the flux at each wavelength is divided by the maximum flux in that spectrum) and the spectra are then offset from each other along the y-axis to make the plot easier to view. The colour of the lines between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe hotter stars have more of their flux at the bluer end of the spectrum and the cooler stars have more of their flux at the redder end. However the total amount of flux a star emits depends on its size and temperature. Due to this, a hot star will emit more red light than a cool star of the same size even if the cool star emits almost all its light in red light but this is not visible in this plot due to the normalization mentioned above. The sharp, narrow drops in the spectra are absorption lines caused by atoms and ions in the stars’ atmospheres. The strength of a spectral line depends on the temperature of a star’s atmosphere. Take the hydrogen line at 656.5 nm as an example. All of the stars in this plot are primarily made of hydrogen, but the 656.5 nm hydrogen line is weak for the hottest and coolest stars but strongest for spectral types A and F. This is because hydrogen absorbs more light at 656.5 nm at the temperatures of A and F stars’ atmospheres than in hotter or cooler stars.\r\n\r\nThe coolest star here, the M-type star, has wide absorption bands in its spectra. This is because this star is cool enough to have compounds such as titanium oxide in its atmosphere. These compounds, often called molecules in astronomy, produce wider spectral absorption features than atoms or ions.",
"alt_text": "Seven lines. The peak of each line moves from short wavelengths for the top line to longer wavelengths for the bottom line.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-lines_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-lines_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/Tt35DR10iI63/"
},
{
"diagram_label": "Stellar spectral types - bands",
"diagram_slug": "W970mQ74LZ29",
"diagram_title": "Stellar spectral types - bands",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "The spectra of seven stars ordered by spectral type ranging from the hottest (O-type) at the top to the coolest (M-type at the bottom). The x-axis shows the wavelength of light while the brightness or darkness at each wavelength corresponds to the flux of light received from the star at that wavelength with darker patches having less flux and brighter patches more. Each spectrum is normalized (the flux at each wavelength is divided by the maximum flux for that spectrum) so that the maximum flux should appear with the same brightness for all the spectra. The colour plotted between 400 nm and 700 nm roughly corresponds to the color the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.\r\n\r\nThe hotter stars have more of their flux at the bluer end of the spectrum and the cooler stars have more of their flux at the redder end. However the total amount of flux a star emits depends on its size and temperature. Due to this, a hot star will emit more red light than a cool star of the same size even if the cool star emits almost all its light in red light but this is not visible in this plot due to the normalization mentioned above. The dark, narrow patches in the spectra are absorption lines caused by atoms and ions in the stars’ atmospheres. The strength of a spectral line depends on the temperature of a star’s atmosphere. Take the hydrogen line at 656.5 nm as an example. All of the stars in this plot are primarily made of hydrogen, but the 656.5 nm hydrogen line is weak for the hottest and coolest stars but strongest for spectral types A and F. This is because hydrogen absorbs more light at 656.5 nm at the temperatures of A and F stars’ atmospheres than in hotter or cooler stars.\r\n\r\nThe coolest star here, the M-type star, has wide absorption bands in its spectra. This is because this star is cool enough to have compounds such as titanium oxide in its atmosphere. These compounds, often called molecules in astronomy, produce wider spectral absorption features than atoms or ions.",
"alt_text": "Seven bands with bright and dark patches. The brightest part of the band moves from blue in the top band to red at the bottom",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-bands_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-bands_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/W970mQ74LZ29/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "Radiazione di corpo nero",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Le curve della radiazione emessa da corpi neri di diversa temperatura. L'asse delle ascisse indica la lunghezza d'onda e l'asse delle ordinate la quantità di energia emessa ogni secondo da un metro quadrato della superficie di quel corpo nero a ciascuna lunghezza d'onda.\r\n\r\nQuanto più caldo è il corpo, tanto più corta è la lunghezza d'onda e tanto più blu è la luce a cui emette la massima quantità di energia. Nonostante il corpo più freddo in questo grafico abbia un picco di luce rossa, gli altri corpi più caldi emettono tutti più luce rossa rispetto al corpo più freddo.",
"alt_text": "Tre curve con radiazione sull'asse y e lunghezza d'onda sull'asse x. Le curve più fredde hanno picchi più rossi e più bassi.",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "Radiazione di corpo nero - Catastrofe UV",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Le curve della radiazione emessa da corpi neri di diversa temperatura. L'asse delle ascisse indica la lunghezza d'onda e l'asse delle ordinate la quantità di energia emessa ogni secondo da un metro quadrato della superficie di quel corpo nero a ciascuna lunghezza d'onda.\r\n\r\nQuanto più caldo è il corpo, tanto più corta è la lunghezza d'onda e tanto più blu è la luce a cui emette la massima quantità di energia. Nonostante il corpo più freddo in questo grafico abbia un picco di luce rossa, gli altri corpi più caldi emettono tutti più luce rossa rispetto al corpo più freddo.\r\n\r\nLa linea tratteggiata mostra la radiazione emessa prevista dalla teoria classica prima della moderna meccanica quantistica. Questa previsione tende all'infinito alle lunghezze d'onda più corte per qualsiasi temperatura del corpo nero superiore allo zero ed è stata soprannominata \"catastrofe ultravioletta\".",
"alt_text": "Tre curve con radiazione sull'asse y e lunghezza d'onda sull'asse x. Le curve più fredde hanno picchi più rossi e più bassi.",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Spectrum of an O-type star",
"diagram_slug": "m5801x5SA50",
"diagram_title": "Spettro di una stella di tipo O",
"glossary_terms": [
328,
382,
463
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Spettro della stella di tipo O HD 235673 con lunghezza d'onda in nanometri sull'asse x e flusso sull'asse y. La parte superiore del grafico mostra lo stesso spettro, ma con macchie chiare per le lunghezze d'onda ad alto flusso e macchie scure per le lunghezze d'onda a basso flusso. Il colore della linea tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe righe nere mostrano le linee di assorbimento spettrale causate da atomi e ioni di diversi elementi presenti nell'atmosfera della stella. Questi atomi e ioni assorbono a lunghezze d'onda specifiche, causando linee scure e nitide nello spettro. La densità di queste righe dipende dalla temperatura dell'atmosfera della stella. Due stelle composte dalla stessa miscela di elementi potrebbero avere spettri con serie di righe molto diverse se le loro atmosfere hanno temperature diverse. Per le stelle di tipo O le caratteristiche più importanti sono un piccolo numero di linee causate dall'elio ionizzato. Queste righe sono più marcate nelle stelle di tipo O che in quelle più fredde. Nello spettro compaiono anche linee di atomi di elio e di idrogeno. Lo spettro presenta un flusso maggiore all'estremità blu dello spettro rispetto a quella rossa.",
"alt_text": "Una linea liscia che declina a lunghezze d'onda maggiori con alcuni bruschi avvallamenti.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-o-type-star_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-o-type-star_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/m5801x5SA50/"
},
{
"diagram_label": "Spectrum of a B-type star",
"diagram_slug": "QF74Q764Tb95",
"diagram_title": "Spettro di una stella di tipo B",
"glossary_terms": [
37,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Lo spettro della stella di tipo B HD 258982. Il colore della linea tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe righe nere mostrano le linee di assorbimento spettrale causate da atomi e ioni di diversi elementi presenti nell'atmosfera della stella. Questi atomi e ioni assorbono a lunghezze d'onda specifiche, ingenerando linee scure e nitide nello spettro. La densità di queste righe dipende dalla temperatura dell'atmosfera della stella. Due stelle composte dalla stessa miscela di elementi potrebbero avere spettri con serie di linee molto diverse se le loro atmosfere hanno temperature diverse. Per le stelle di tipo B le linee più importanti sono causate dagli atomi di elio. Queste righe sono più marcate nelle stelle di tipo B e più deboli nei tipi più caldi e più freddi. Ci sono anche le righe degli atomi di idrogeno, ma non sono così marcate come nelle stelle di tipo A più fredde.",
"alt_text": "Una linea liscia che declina a lunghezze d'onda maggiori con qualche brusco calo.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-b-type-star_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-b-type-star_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/QF74Q764Tb95/"
},
{
"diagram_label": "Spectrum of an A-type star",
"diagram_slug": "2149RS77wy92",
"diagram_title": "Spettro di una stella di tipo A",
"glossary_terms": [
1,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Lo spettro della stella di tipo A BD-11 1212. Il colore della linea tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe righe nere mostrano le linee di assorbimento spettrale causate da atomi e ioni di diversi elementi presenti nell'atmosfera della stella. Questi atomi e ioni assorbono a lunghezze d'onda specifiche, ingenerando linee scure e nitide nello spettro. La densità di queste righe dipende dalla temperatura dell'atmosfera della stella. Due stelle composte dalla stessa miscela di elementi potrebbero avere spettri con serie di linee molto diverse se le loro atmosfere hanno temperature diverse. Le linee degli atomi di idrogeno dominano gli spettri delle stelle di tipo A e sono le più forti in questo tipo di spettro.",
"alt_text": "Una linea liscia che raggiunge un picco a circa 420 nm e poi diminuisce a lunghezze d'onda maggiori con alcuni avvallamenti piuttosto ampi.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-a-type-star_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-a-type-star_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/2149RS77wy92/"
},
{
"diagram_label": "Spectrum of an F-type star",
"diagram_slug": "zY580V14PE47",
"diagram_title": "Spettro di una stella di tipo F",
"glossary_terms": [
110,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Lo spettro della stella di tipo F 2MASS J22243289+4937443. Il colore della linea tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe righe nere mostrano le linee di assorbimento spettrale causate da atomi e ioni di diversi elementi presenti nell'atmosfera della stella. Questi atomi e ioni assorbono a lunghezze d'onda specifiche, causando linee scure e nitide nello spettro. La densità di queste righe dipende dalla temperatura dell'atmosfera della stella. Due stelle composte dalla stessa miscela di elementi potrebbero avere spettri con serie di linee molto diverse se le loro atmosfere hanno temperature diverse. Le linee degli atomi di idrogeno, più forti nelle stelle di tipo A, sono ancora relativamente forti nelle stelle di tipo F, ma le linee dei metalli, in particolare del calcio ionizzato, iniziano a diventare forti a questo tipo di spettro.",
"alt_text": "Una linea relativamente liscia che raggiunge un picco a circa 430 nm e poi diminuisce a lunghezze d'onda maggiori con avvallamenti piuttosto ampi.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-f-type-star_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-f-type-star_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/zY580V14PE47/"
},
{
"diagram_label": "Spectrum of a G-type star",
"diagram_slug": "mX21es50Pj16",
"diagram_title": "Spettro di una stella di tipo G",
"glossary_terms": [
328,
382,
442
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Lo spettro della stella di tipo G UCAC4 700-069569. Il colore della linea tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe righe nere mostrano le linee di assorbimento spettrale causate da atomi e ioni di diversi elementi presenti nell'atmosfera della stella. Questi atomi e ioni assorbono a lunghezze d'onda specifiche, causando linee scure e nitide nello spettro. La densità di queste righe dipende dalla temperatura dell'atmosfera della stella. Due stelle composte dalla stessa miscela di elementi potrebbero avere spettri con serie di linee molto diverse se le loro atmosfere hanno temperature diverse. Nelle stelle di tipo G le linee degli atomi di idrogeno sono più deboli rispetto alle stelle di tipo F, mentre quelle del calcio ionizzato sono più forti. Anche le linee degli atomi metallici, come gli atomi di ferro, sodio e calcio, iniziano a diventare prominenti.",
"alt_text": "Una linea piuttosto irregolare che raggiunge un picco a circa 470 nm e poi diminuisce a lunghezze d'onda maggiori con alcuni profondi cali.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-g-type-star_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-g-type-star_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/mX21es50Pj16/"
},
{
"diagram_label": "Spectrum of a K-type star",
"diagram_slug": "lH42QC364e69",
"diagram_title": "Spettro di una stella di tipo K",
"glossary_terms": [
168,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Lo spettro della stella di tipo K 2MASS J19554455+4754531. Il colore della linea tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe righe nere mostrano le linee di assorbimento spettrale causate da atomi e ioni di diversi elementi presenti nell'atmosfera della stella. Questi atomi e ioni assorbono a lunghezze d'onda specifiche, causando linee scure e nitide nello spettro. La densità di queste righe dipende dalla temperatura dell'atmosfera della stella. Due stelle composte dalla stessa miscela di elementi potrebbero avere spettri con serie di linee molto diverse se le loro atmosfere hanno temperature diverse. Gli spettri delle stelle di tipo K sono dominati da atomi metallici come quelli di ferro, sodio e calcio. Le righe degli atomi metallici sono talmente tante, troppe da poter essere marcate singolarmente, che lo spettro ha un aspetto irregolare e disordinato. Le linee degli atomi di idrogeno e degli ioni di calcio sono molto più deboli rispetto alle stelle di tipo G, più calde.",
"alt_text": "Una linea irregolare che raggiunge un picco a circa 580 nm e poi diminuisce a lunghezze d'onda maggiori con qualche avvallamento più profondo.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-k-type-star_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-k-type-star_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/lH42QC364e69/"
},
{
"diagram_label": "Spectrum of an M-type star",
"diagram_slug": "d156Ob46Ih98",
"diagram_title": "Spettro di una stella di tipo M",
"glossary_terms": [
328,
382,
453
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Lo spettro della stella di tipo M 2MASS J15581272+8457104. Il colore della linea tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe righe nere mostrano le linee di assorbimento spettrale causate da atomi, ioni e molecole di diversi elementi presenti nell'atmosfera della stella. Questi atomi, ioni e molecole assorbono a lunghezze d'onda specifiche, ingenerando linee scure e nitide nello spettro. La densità di queste linee dipende dalla temperatura dell'atmosfera della stella. Due stelle composte dalla stessa miscela di elementi potrebbero avere spettri con serie di linee molto diverse se le loro atmosfere hanno temperature diverse. Le atmosfere delle stelle di tipo M sono abbastanza fredde da permettere la formazione di alcuni composti chimici. In astronomia si parla spesso di molecole, anche se non si tratta di molecole propriamente chimiche. Queste molecole producono così tante linee nello spettro di una stella di tipo M che le linee sembrano fondersi insieme in bande enormi che eliminano grandi porzioni dallo spettro. Nelle stelle di tipo M, l'ossido di titanio presenta un gran numero di queste bande nella luce visibile, dominando vaste regioni dello spettro.",
"alt_text": "Una linea irregolare che aumenta a lunghezze d'onda maggiori, con ampi avvallamenti e alcuni avvallamenti più netti.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-m-type-star_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-m-type-star_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/d156Ob46Ih98/"
},
{
"diagram_label": "Stellar spectral types",
"diagram_slug": "Tt35DR10iI63",
"diagram_title": "Tipi spettrali stellari",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Gli spettri di sette stelle ordinati per tipo spettrale, dal più caldo (tipo O) in alto al più freddo (tipo M in basso). L'asse delle ascisse indica la lunghezza d'onda della luce e l'asse delle ordinate misura il flusso di luce ricevuto a quella lunghezza d'onda. Ogni spettro viene normalizzato (il flusso a ciascuna lunghezza d'onda viene diviso per il flusso massimo in quello spettro) e gli spettri vengono poi sfalsati l'uno dall'altro lungo l'asse y per rendere il grafico più facile da visualizzare. Il colore delle linee tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe stelle più calde hanno un flusso maggiore all'estremità blu dello spettro, mentre quelle più fredde hanno un flusso maggiore all'estremità rossa. Tuttavia, la quantità totale di flusso emesso da una stella dipende dalle sue dimensioni e dalla sua temperatura. Per questo motivo, una stella calda emetterà più luce rossa di una stella fredda della stessa dimensione, anche se la stella fredda emette quasi tutta la sua luce in rosso, ma questo non è visibile in questo grafico a causa della normalizzazione di cui sopra. Le gocce strette e nette negli spettri sono linee di assorbimento causate da atomi e ioni nell'atmosfera delle stelle. L'intensità di una linea spettrale dipende dalla temperatura dell'atmosfera di una stella. Prendiamo ad esempio la linea dell'idrogeno a 656,5 nm. Tutte le stelle in questo grafico sono costituite principalmente da idrogeno, ma la linea dell'idrogeno a 656,5 nm è sottile per le stelle più calde e più fredde, mentre è più marcata per i tipi spettrali A e F. Questo perché l'idrogeno assorbe più luce a 656,5 nm alle temperature delle atmosfere delle stelle A e F rispetto alle stelle più calde o più fredde.\r\n\r\nLa stella più fredda, quella di tipo M, presenta ampie bande di assorbimento nel suo spettro. Ciò è dovuto al fatto che questa stella è abbastanza fredda da avere composti come l'ossido di titanio nella sua atmosfera. Questi composti, spesso chiamati molecole in astronomia, producono righe di assorbimento spettrale più ampie rispetto agli atomi o agli ioni.",
"alt_text": "Sette linee. Il picco di ciascuna linea passa da lunghezze d'onda brevi per la linea superiore a lunghezze d'onda maggiori per la linea inferiore.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-lines_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-lines_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/Tt35DR10iI63/"
},
{
"diagram_label": "Stellar spectral types - bands",
"diagram_slug": "W970mQ74LZ29",
"diagram_title": "Tipi spettrali stellari - bande",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Gli spettri di sette stelle ordinati per tipo spettrale, dal più caldo (tipo O) in alto al più freddo (tipo M in basso). L'asse delle ascisse mostra la lunghezza d'onda della luce, mentre la luminosità o l'oscurità a ciascuna lunghezza d'onda corrisponde al flusso di luce ricevuto dalla stella a quella lunghezza d'onda, con le macchie più scure che hanno un flusso minore e quelle più luminose maggiore. Ogni spettro è normalizzato (il flusso a ogni lunghezza d'onda è diviso per il flusso massimo per quello spettro) in modo che il flusso massimo appaia con la stessa luminosità per tutti gli spettri. Il colore tracciato tra 400 e 700 nm corrisponde approssimativamente al colore con cui l'occhio umano vede la luce di quella lunghezza d'onda. Al di sotto dei 400 nm e al di sopra dei 700 nm, dove l'occhio umano può vedere poca o nessuna luce, le linee sono colorate rispettivamente di blu e di rosso.\r\n\r\nLe stelle più calde hanno un flusso maggiore all'estremità blu dello spettro, mentre quelle più fredde hanno un flusso maggiore all'estremità rossa. Tuttavia, la quantità totale di flusso emesso da una stella dipende dalle sue dimensioni e dalla sua temperatura. Per questo motivo, una stella calda emetterà più luce rossa di una stella fredda della stessa dimensione, anche se la stella fredda emette quasi tutta la sua luce in rosso, ma questo non è visibile in questo grafico a causa della normalizzazione di cui sopra. Le macchie scure e strette negli spettri sono linee di assorbimento causate da atomi e ioni nell'atmosfera delle stelle. L'intensità di una linea spettrale dipende dalla temperatura dell'atmosfera di una stella. Prendiamo ad esempio la linea dell'idrogeno a 656,5 nm. Tutte le stelle in questo grafico sono costituite principalmente da idrogeno, ma la linea dell'idrogeno a 656,5 nm è debole per le stelle più calde e più fredde, mentre è più forte per i tipi spettrali A e F. Questo perché l'idrogeno assorbe più luce a 656,5 nm alle temperature delle atmosfere delle stelle A e F rispetto alle stelle più calde o più fredde.\r\n\r\nLa stella più fredda, quella di tipo M, presenta ampie bande di assorbimento nel suo spettro. Ciò è dovuto al fatto che questa stella è abbastanza fredda da avere composti come l'ossido di titanio nella sua atmosfera. Questi composti, spesso definiti molecole in astronomia, producono righe di assorbimento spettrale più ampie rispetto agli atomi o agli ioni.",
"alt_text": "Sette bande con macchie chiare e scure. La parte più luminosa della banda passa dal blu della banda superiore al rosso della banda inferiore.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-bands_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-bands_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/W970mQ74LZ29/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "Rayonnement du corps noir",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Courbes du rayonnement émis par des corps noirs de différentes températures. L'axe des x indique la longueur d'onde et l'axe des y indique la quantité d'énergie émise chaque seconde par un mètre carré de la surface de ce corps noir à chaque longueur d'onde.\r\n\r\nPlus le corps est chaud, plus la longueur d'onde est courte et plus la lumière qu'il émet est bleue. Bien que le corps le plus froid de ce diagramme atteigne un pic de lumière rouge, les autres corps plus chauds émettent tous plus de lumière rouge que le corps le plus froid.",
"alt_text": "Trois courbes avec le rayonnement sur l'axe y et la longueur d'onde sur l'axe x. Les courbes les plus froides ont des pics plus rouges et plus bas.",
"credit_text": "AIU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "Rayonnement du corps noir - Catastrophe UV",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Courbes du rayonnement émis par des corps noirs de différentes températures. L'axe des x indique la longueur d'onde et l'axe des y indique la quantité d'énergie émise chaque seconde par un mètre carré de la surface de ce corps noir à chaque longueur d'onde.\r\n\r\nPlus le corps est chaud, plus la longueur d'onde est courte et plus la lumière qu'il émet est bleue. Bien que le corps le plus froid de ce diagramme atteigne un pic de lumière rouge, les autres corps plus chauds émettent tous plus de lumière rouge que le corps le plus froid.\r\n\r\nLa ligne en pointillé montre le rayonnement émis prédit par la théorie classique avant la mécanique quantique moderne. Cette prédiction tend vers l'infini aux courtes longueurs d'onde pour toute température du corps noir supérieure à zéro et a été surnommée la \"catastrophe ultraviolette\".",
"alt_text": "Trois courbes avec le rayonnement sur l'axe y et la longueur d'onde sur l'axe x. Les courbes les plus froides ont des pics plus rouges et plus bas.",
"credit_text": "AIU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Spectrum of an O-type star",
"diagram_slug": "m5801x5SA50",
"diagram_title": "Spectre d'une étoile de type O",
"glossary_terms": [
328,
382,
463
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Spectre de l'étoile de type O HD 235673 avec la longueur d'onde en nanomètres sur l'axe des x et le flux sur l'axe des y. La partie supérieure du graphique montre le même spectre, mais avec des taches claires pour les longueurs d'onde à flux élevé et des taches sombres pour les longueurs d'onde à faible flux. La couleur de la ligne entre 400 nm et 700 nm correspond approximativement à la couleur de la lumière de cette longueur d'onde perçue par l'œil humain. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes lignes noires montrent les lignes d'absorption spectrale causées par les atomes et les ions de différents éléments présents dans l'atmosphère de l'étoile. Ces atomes et ions absorbent à des longueurs d'onde spécifiques, ce qui provoque des lignes sombres et nettes dans les spectres. L'intensité de ces lignes dépend de la température de l'atmosphère de l'étoile. Deux étoiles composées du même mélange d'éléments peuvent présenter des spectres avec des jeux de raies très différents si leurs atmosphères ont des températures différentes. Pour les étoiles de type O, les caractéristiques les plus importantes sont un petit nombre de raies causées par l'hélium ionisé. Ces raies sont plus intenses dans les étoiles de type O que dans les étoiles plus froides. Des raies provenant d'atomes d'hélium et d'hydrogène apparaissent également dans le spectre. Le spectre présente un flux plus important à l'extrémité bleue du spectre qu'à l'extrémité rouge.",
"alt_text": "Une ligne lisse qui décroît à des longueurs d'onde plus longues avec quelques creux importants.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-o-type-star_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-o-type-star_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/m5801x5SA50/"
},
{
"diagram_label": "Spectrum of a B-type star",
"diagram_slug": "QF74Q764Tb95",
"diagram_title": "Spectre d'une étoile de type B",
"glossary_terms": [
37,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Le spectre de l'étoile de type B HD 258982. La couleur de la raie entre 400 nm et 700 nm correspond approximativement à la couleur de la lumière que l'œil humain verrait à cette longueur d'onde. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes lignes noires montrent les lignes d'absorption spectrale causées par les atomes et les ions de différents éléments présents dans l'atmosphère de l'étoile. Ces atomes et ions absorbent à des longueurs d'onde spécifiques, ce qui provoque des raies sombres et nettes dans les spectres. L'intensité de ces lignes dépend de la température de l'atmosphère de l'étoile. Deux étoiles composées du même mélange d'éléments peuvent présenter des spectres avec des jeux de raies très différents si leurs atmosphères ont des températures différentes. Pour les étoiles de type B, les raies les plus importantes sont causées par les atomes d'hélium. Ces raies sont les plus fortes dans les étoiles de type B et les plus faibles dans les étoiles plus chaudes et plus froides. Les raies dues aux atomes d'hydrogène sont également présentes mais ne sont pas aussi fortes que dans les étoiles de type A plus froides.",
"alt_text": "Une ligne lisse décroissant à des longueurs d'onde plus longues avec quelques creux marqués.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-b-type-star_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-b-type-star_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/QF74Q764Tb95/"
},
{
"diagram_label": "Spectrum of an A-type star",
"diagram_slug": "2149RS77wy92",
"diagram_title": "Spectre d'une étoile de type A",
"glossary_terms": [
1,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Le spectre de l'étoile de type A BD-11 1212. La couleur de la ligne entre 400 nm et 700 nm correspond approximativement à la couleur de la lumière que l'œil humain verrait à cette longueur d'onde. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes lignes noires montrent les lignes d'absorption spectrale causées par les atomes et les ions de différents éléments présents dans l'atmosphère de l'étoile. Ces atomes et ions absorbent à des longueurs d'onde spécifiques, ce qui provoque des lignes sombres et nettes dans les spectres. L'intensité de ces lignes dépend de la température de l'atmosphère de l'étoile. Deux étoiles composées du même mélange d'éléments peuvent présenter des spectres avec des jeux de raies très différents si leurs atmosphères ont des températures différentes. Les raies des atomes d'hydrogène dominent les spectres des étoiles de type A et sont les plus intenses dans ce type spectral.",
"alt_text": "Une ligne régulière culminant à environ 420 nm puis diminuant à des longueurs d'onde plus élevées avec quelques creux assez larges.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-a-type-star_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-a-type-star_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/2149RS77wy92/"
},
{
"diagram_label": "Spectrum of an F-type star",
"diagram_slug": "zY580V14PE47",
"diagram_title": "Spectre d'une étoile de type F",
"glossary_terms": [
110,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Le spectre de l'étoile de type F 2MASS J22243289+4937443. La couleur de la raie entre 400 nm et 700 nm correspond approximativement à la couleur de la lumière que l'œil humain verrait à cette longueur d'onde. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes lignes noires montrent les lignes d'absorption spectrale causées par les atomes et les ions de différents éléments présents dans l'atmosphère de l'étoile. Ces atomes et ions absorbent à des longueurs d'onde spécifiques, ce qui provoque des lignes sombres et nettes dans les spectres. L'intensité de ces lignes dépend de la température de l'atmosphère de l'étoile. Deux étoiles composées du même mélange d'éléments peuvent présenter des spectres avec des jeux de raies très différents si leurs atmosphères ont des températures différentes. Les raies des atomes d'hydrogène, qui sont les plus intenses dans les étoiles de type A, sont encore relativement intenses dans les étoiles de type F, mais les raies des métaux, en particulier du calcium ionisé, commencent à devenir intenses dans ce type de spectre.",
"alt_text": "Une ligne relativement lisse culminant à environ 430 nm puis diminuant à des longueurs d'onde plus élevées avec quelques creux assez larges.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-f-type-star_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-f-type-star_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/zY580V14PE47/"
},
{
"diagram_label": "Spectrum of a G-type star",
"diagram_slug": "mX21es50Pj16",
"diagram_title": "Spectre d'une étoile de type G",
"glossary_terms": [
328,
382,
442
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Le spectre de l'étoile de type G UCAC4 700-069569. La couleur de la ligne entre 400 nm et 700 nm correspond approximativement à la couleur de la lumière que l'œil humain verrait à cette longueur d'onde. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes lignes noires montrent les lignes d'absorption spectrale causées par les atomes et les ions de différents éléments présents dans l'atmosphère de l'étoile. Ces atomes et ions absorbent à des longueurs d'onde spécifiques, ce qui provoque des raies sombres et nettes dans les spectres. L'intensité de ces lignes dépend de la température de l'atmosphère de l'étoile. Deux étoiles composées du même mélange d'éléments peuvent présenter des spectres avec des jeux de raies très différents si leurs atmosphères ont des températures différentes. Dans les étoiles de type G, les raies des atomes d'hydrogène sont plus faibles que dans les étoiles de type F et les raies du calcium ionisé plus fortes. Les raies des atomes métalliques tels que les atomes de fer, de sodium et de calcium commencent également à devenir proéminentes.",
"alt_text": "Une ligne assez irrégulière culminant à environ 470 nm puis déclinant à des longueurs d'onde plus grandes avec quelques creux plus profonds.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-g-type-star_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-g-type-star_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/mX21es50Pj16/"
},
{
"diagram_label": "Spectrum of a K-type star",
"diagram_slug": "lH42QC364e69",
"diagram_title": "Spectre d'une étoile de type K",
"glossary_terms": [
168,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Le spectre de l'étoile de type K 2MASS J19554455+4754531. La couleur de la raie entre 400 nm et 700 nm correspond approximativement à la couleur de la lumière que l'œil humain verrait à cette longueur d'onde. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes lignes noires montrent les lignes d'absorption spectrale causées par les atomes et les ions de différents éléments présents dans l'atmosphère de l'étoile. Ces atomes et ions absorbent à des longueurs d'onde spécifiques, ce qui provoque des lignes sombres et nettes dans les spectres. L'intensité de ces lignes dépend de la température de l'atmosphère de l'étoile. Deux étoiles composées du même mélange d'éléments peuvent présenter des spectres avec des jeux de raies très différents si leurs atmosphères ont des températures différentes. Les spectres des étoiles de type K sont dominés par les atomes métalliques tels que les atomes de fer, de sodium et de calcium. Les atomes métalliques sont à l'origine d'un si grand nombre de raies, bien trop nombreuses pour être marquées individuellement, que le spectre a une apparence hachée et irrégulière. Les raies des atomes d'hydrogène et des ions calcium sont beaucoup plus faibles que dans les étoiles de type G, plus chaudes.",
"alt_text": "Une ligne irrégulière culminant à environ 580 nm puis déclinant à des longueurs d'onde plus grandes avec quelques creux plus profonds.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-k-type-star_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-k-type-star_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/lH42QC364e69/"
},
{
"diagram_label": "Spectrum of an M-type star",
"diagram_slug": "d156Ob46Ih98",
"diagram_title": "Spectre d'une étoile de type M",
"glossary_terms": [
328,
382,
453
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Le spectre de l'étoile de type M 2MASS J15581272+8457104. La couleur de la raie entre 400 nm et 700 nm correspond approximativement à la couleur de la lumière que l'œil humain verrait à cette longueur d'onde. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes lignes noires montrent les lignes d'absorption spectrale causées par les atomes, les ions et les molécules de différents éléments présents dans l'atmosphère de l'étoile. Ces atomes, ions et molécules absorbent à des longueurs d'onde spécifiques, ce qui provoque des lignes sombres et nettes dans les spectres. L'intensité de ces raies dépend de la température de l'atmosphère de l'étoile. Deux étoiles composées du même mélange d'éléments peuvent présenter des spectres avec des jeux de raies très différents si leurs atmosphères ont des températures différentes. L'atmosphère des étoiles de type M est suffisamment froide pour permettre la formation de certains composés chimiques. Ceux-ci sont souvent appelés molécules en astronomie, même s'il ne s'agit pas à proprement parler de molécules en chimie. Ces molécules produisent tellement de raies dans le spectre d'une étoile de type M que les raies semblent fusionner en d'immenses bandes qui éliminent de grandes parties du spectre. Dans les étoiles de type M, l'oxyde de titane présente un grand nombre de ces bandes dans la lumière visible, dominant de vastes régions du spectre.",
"alt_text": "Une ligne irrégulière augmentant à de plus grandes longueurs d'onde avec de larges creux et quelques creux plus marqués.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-m-type-star_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-m-type-star_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/d156Ob46Ih98/"
},
{
"diagram_label": "Stellar spectral types",
"diagram_slug": "Tt35DR10iI63",
"diagram_title": "Types spectraux stellaires",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Les spectres de sept étoiles classés par type spectral, du plus chaud (type O) en haut au plus froid (type M en bas). L'axe des x indique la longueur d'onde de la lumière et l'axe des y est une mesure du flux de lumière reçu à cette longueur d'onde. Chaque spectre est normalisé (le flux à chaque longueur d'onde est divisé par le flux maximal dans ce spectre) et les spectres sont ensuite décalés les uns par rapport aux autres le long de l'axe des y pour faciliter la visualisation du graphique. La couleur des lignes entre 400 nm et 700 nm correspond approximativement à la couleur de la lumière de cette longueur d'onde perçue par l'œil humain. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes étoiles les plus chaudes ont un flux plus important à l'extrémité bleue du spectre et les étoiles les plus froides ont un flux plus important à l'extrémité rouge. Toutefois, la quantité totale de flux émis par une étoile dépend de sa taille et de sa température. Ainsi, une étoile chaude émettra plus de lumière rouge qu'une étoile froide de même taille, même si l'étoile froide émet presque toute sa lumière dans le rouge, mais cela n'est pas visible sur ce graphique en raison de la normalisation mentionnée ci-dessus. Les gouttes étroites et nettes dans les spectres sont des raies d'absorption causées par les atomes et les ions dans l'atmosphère des étoiles. L'intensité d'une raie spectrale dépend de la température de l'atmosphère de l'étoile. Prenons par exemple la raie de l'hydrogène à 656,5 nm. Toutes les étoiles de ce graphique sont principalement composées d'hydrogène, mais la raie de l'hydrogène à 656,5 nm est faible pour les étoiles les plus chaudes et les plus froides, mais plus forte pour les types spectraux A et F. Cela s'explique par le fait que l'hydrogène absorbe plus de lumière à 656,5 nm aux températures de l'atmosphère des étoiles A et F que dans les étoiles les plus chaudes ou les plus froides.\r\n\r\nL'étoile la plus froide, l'étoile de type M, présente de larges bandes d'absorption dans ses spectres. Cela s'explique par le fait que cette étoile est suffisamment froide pour que son atmosphère contienne des composés tels que l'oxyde de titane. Ces composés, souvent appelés molécules en astronomie, produisent des caractéristiques d'absorption spectrale plus larges que les atomes ou les ions.",
"alt_text": "Sept lignes. Le pic de chaque ligne passe des courtes longueurs d'onde pour la ligne supérieure aux grandes longueurs d'onde pour la ligne inférieure.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-lines_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-lines_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/Tt35DR10iI63/"
},
{
"diagram_label": "Stellar spectral types - bands",
"diagram_slug": "W970mQ74LZ29",
"diagram_title": "Types spectraux stellaires - bandes",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Les spectres de sept étoiles classés par type spectral, du plus chaud (type O) en haut au plus froid (type M en bas). L'axe des x indique la longueur d'onde de la lumière, tandis que la luminosité ou l'obscurité à chaque longueur d'onde correspond au flux de lumière reçu de l'étoile à cette longueur d'onde, les taches plus sombres ayant un flux plus faible et les taches plus lumineuses un flux plus important. Chaque spectre est normalisé (le flux à chaque longueur d'onde est divisé par le flux maximal pour ce spectre) afin que le flux maximal apparaisse avec la même luminosité pour tous les spectres. La couleur représentée entre 400 nm et 700 nm correspond approximativement à la couleur que l'œil humain verrait pour la lumière de cette longueur d'onde. En dessous de 400 nm et au-dessus de 700 nm, où l'œil humain ne voit que peu ou pas de lumière, les lignes sont colorées respectivement en bleu et en rouge.\r\n\r\nLes étoiles les plus chaudes ont un flux plus important à l'extrémité bleue du spectre et les étoiles les plus froides ont un flux plus important à l'extrémité rouge. Toutefois, la quantité totale de flux émis par une étoile dépend de sa taille et de sa température. Ainsi, une étoile chaude émettra plus de lumière rouge qu'une étoile froide de même taille, même si l'étoile froide émet presque toute sa lumière dans le rouge, mais cela n'est pas visible sur ce graphique en raison de la normalisation mentionnée ci-dessus. Les taches sombres et étroites dans les spectres sont des lignes d'absorption causées par les atomes et les ions dans l'atmosphère des étoiles. L'intensité d'une raie spectrale dépend de la température de l'atmosphère de l'étoile. Prenons par exemple la raie de l'hydrogène à 656,5 nm. Toutes les étoiles de ce graphique sont principalement composées d'hydrogène, mais la raie de l'hydrogène à 656,5 nm est faible pour les étoiles les plus chaudes et les plus froides, mais plus forte pour les types spectraux A et F. Cela s'explique par le fait que l'hydrogène absorbe plus de lumière à 656,5 nm aux températures de l'atmosphère des étoiles A et F que dans les étoiles les plus chaudes ou les plus froides.\r\n\r\nL'étoile la plus froide, l'étoile de type M, présente de larges bandes d'absorption dans ses spectres. Cela s'explique par le fait que cette étoile est suffisamment froide pour que son atmosphère contienne des composés tels que l'oxyde de titane. Ces composés, souvent appelés molécules en astronomie, produisent des caractéristiques d'absorption spectrale plus larges que les atomes ou les ions.",
"alt_text": "Sept bandes avec des zones lumineuses et sombres. La partie la plus brillante du bandeau passe du bleu dans le haut au rouge en bas.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-bands_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-bands_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/W970mQ74LZ29/"
},
{
"diagram_label": "Spectrum of an O-type star",
"diagram_slug": "m5801x5SA50",
"diagram_title": "Espectro de una estrella tipo O",
"glossary_terms": [
328,
382,
463
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectro de la estrella tipo O HD 235673 con la longitud de onda en nanómetros en el eje de abscisas y el flujo en el eje de ordenadas. La parte superior del gráfico muestra el mismo espectro, pero con zonas brillantes para las longitudes de onda de alto flujo y zonas oscuras para las longitudes de onda de bajo flujo. El color de la línea entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas líneas negras muestran las líneas de absorción espectral causadas por átomos e iones de diferentes elementos de la atmósfera de la estrella. Estos átomos e iones absorben en longitudes de onda específicas, provocando líneas nítidas y oscuras en el espectro. La intensidad de estas líneas depende de la temperatura de la atmósfera de la estrella. Dos estrellas formadas por la misma mezcla de elementos pueden tener espectros con conjuntos de líneas muy diferentes si sus atmósferas tienen temperaturas distintas. En las estrellas tipo O, la característica más importante es un pequeño número de líneas causadas por el helio ionizado. Estas líneas son más intensas en las estrellas tipo O que en las estrellas más frías. Las líneas de los átomos de helio y de hidrógeno también aparecen en el espectro. El espectro tiene más flujo en el extremo azul que en el extremo rojo del espectro.",
"alt_text": "Una línea suave que declina a longitudes de onda más largas con algunas caídas bruscas.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-o-type-star_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-o-type-star_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/m5801x5SA50/"
},
{
"diagram_label": "Spectrum of a B-type star",
"diagram_slug": "QF74Q764Tb95",
"diagram_title": "Espectro de una estrella tipo B",
"glossary_terms": [
37,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectro de la estrella tipo B HD 258982. El color de la línea entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas líneas negras muestran las líneas de absorción espectral causadas por átomos e iones de diferentes elementos de la atmósfera de la estrella. Estos átomos e iones absorben en longitudes de onda específicas, provocando líneas nítidas y oscuras en el espectro. La intensidad de estas líneas depende de la temperatura de la atmósfera de la estrella. Dos estrellas formadas por la misma mezcla de elementos pueden tener espectros con conjuntos de líneas muy diferentes si sus atmósferas tienen temperaturas distintas. En las estrellas tipo B, las líneas más importantes son las causadas por los átomos de helio. Estas líneas son más intensas en las estrellas tipo B y más débiles en los tipos más calientes y más fríos. Las líneas de los átomos de hidrógeno también están presentes, pero no son tan intensas como en las estrellas tipo A más frías.",
"alt_text": "Una línea suave que declina a longitudes de onda más largas con algunas caídas bruscas.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-b-type-star_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-b-type-star_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/QF74Q764Tb95/"
},
{
"diagram_label": "Spectrum of an A-type star",
"diagram_slug": "2149RS77wy92",
"diagram_title": "Espectro de una estrella tipo A",
"glossary_terms": [
1,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectro de la estrella tipo A BD-11 1212. El color de la línea entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas líneas negras muestran las líneas de absorción espectral causadas por átomos e iones de diferentes elementos de la atmósfera de la estrella. Estos átomos e iones absorben en longitudes de onda específicas, provocando líneas nítidas y oscuras en el espectro. La intensidad de estas líneas depende de la temperatura de la atmósfera de la estrella. Dos estrellas formadas por la misma mezcla de elementos pueden tener espectros con conjuntos de líneas muy diferentes si sus atmósferas tienen temperaturas distintas. Las líneas de los átomos de hidrógeno dominan los espectros de las estrellas tipo A y son más intensas en este tipo espectral.",
"alt_text": "Una línea suave que alcanza su punto máximo en torno a 420 nm y luego disminuye a longitudes de onda más largas con algunas caídas bastante amplias.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-a-type-star_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-a-type-star_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/2149RS77wy92/"
},
{
"diagram_label": "Spectrum of an F-type star",
"diagram_slug": "zY580V14PE47",
"diagram_title": "Espectro de una estrella tipo F",
"glossary_terms": [
110,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectro de la estrella tipo F 2MASS J22243289+4937443. El color de la línea entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas líneas negras muestran las líneas de absorción espectral causadas por átomos e iones de diferentes elementos de la atmósfera de la estrella. Estos átomos e iones absorben en longitudes de onda específicas, provocando líneas nítidas y oscuras en el espectro. La intensidad de estas líneas depende de la temperatura de la atmósfera de la estrella. Dos estrellas formadas por la misma mezcla de elementos pueden tener espectros con conjuntos de líneas muy diferentes si sus atmósferas tienen temperaturas distintas. Las líneas de los átomos de hidrógeno, que son las más intensas en las estrellas tipo A, siguen siendo relativamente intensas en las estrellas tipo F, pero las líneas de los metales, especialmente del calcio ionizado, empiezan a ser más intensas en este tipo espectral.",
"alt_text": "Una línea relativamente suave con un máximo a los 430 nm que luego disminuye a longitudes de onda más largas con algunas caídas bastante amplias.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-f-type-star_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-f-type-star_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/zY580V14PE47/"
},
{
"diagram_label": "Spectrum of a G-type star",
"diagram_slug": "mX21es50Pj16",
"diagram_title": "Espectro de una estrella tipo G",
"glossary_terms": [
328,
382,
442
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectro de la estrella tipo G UCAC4 700-069569. El color de la línea entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas líneas negras muestran las líneas de absorción espectral causadas por átomos e iones de diferentes elementos de la atmósfera de la estrella. Estos átomos e iones absorben en longitudes de onda específicas, provocando líneas nítidas y oscuras en el espectro. La intensidad de estas líneas depende de la temperatura de la atmósfera de la estrella. Dos estrellas formadas por la misma mezcla de elementos pueden tener espectros con conjuntos de líneas muy diferentes si sus atmósferas tienen temperaturas distintas. En las estrellas tipo G, las líneas de los átomos de hidrógeno son más débiles que en las estrellas tipo F y las líneas del calcio ionizado son más intensas. Las líneas de los átomos metálicos, como los átomos de hierro, sodio y calcio, también empiezan a ser prominentes.",
"alt_text": "Una línea bastante irregular con un máximo en torno a los 470 nm que luego disminuye a longitudes de onda más largas con algunas caídas más profundas.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-g-type-star_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-g-type-star_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/mX21es50Pj16/"
},
{
"diagram_label": "Spectrum of a K-type star",
"diagram_slug": "lH42QC364e69",
"diagram_title": "Espectro de una estrella tipo K",
"glossary_terms": [
168,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectro de la estrella tipo K 2MASS J19554455+4754531. El color de la línea entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas líneas negras muestran las líneas de absorción espectral causadas por átomos e iones de diferentes elementos de la atmósfera de la estrella. Estos átomos e iones absorben en longitudes de onda específicas, provocando líneas nítidas y oscuras en el espectro. La intensidad de estas líneas depende de la temperatura de la atmósfera de la estrella. Dos estrellas formadas por la misma mezcla de elementos pueden tener espectros con conjuntos de líneas muy diferentes si sus atmósferas tienen temperaturas distintas. En los espectros de las estrellas tipo K predominan los átomos metálicos, como los de hierro, sodio y calcio. Hay tantas líneas de átomos metálicos, demasiadas para marcarlas individualmente, que el espectro tiene un aspecto entrecortado y desigual. Las líneas de los átomos de hidrógeno y los iones de calcio son mucho más débiles que en las estrellas tipo G, más calientes.",
"alt_text": "Una línea irregular que alcanza un máximo a 580 nm y luego disminuye a longitudes de onda más largas con algunas caídas más profundas.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-k-type-star_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-k-type-star_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/lH42QC364e69/"
},
{
"diagram_label": "Spectrum of an M-type star",
"diagram_slug": "d156Ob46Ih98",
"diagram_title": "Espectro de una estrella tipo M",
"glossary_terms": [
328,
382,
453
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectro de la estrella tipo M 2MASS J15581272+8457104. El color de la línea entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas líneas negras muestran las líneas de absorción espectral causadas por átomos, iones y moléculas de diferentes elementos de la atmósfera de la estrella. Estos átomos, iones y moléculas absorben en longitudes de onda específicas, provocando líneas nítidas y oscuras en el espectro. La intensidad de estas líneas depende de la temperatura de la atmósfera de la estrella. Dos estrellas formadas por la misma mezcla de elementos pueden tener espectros con conjuntos de líneas muy diferentes si sus atmósferas tienen temperaturas distintas. Las atmósferas de las estrellas tipo M son lo suficientemente frías como para que se formen algunos compuestos químicos. En astronomía, estos compuestos suelen denominarse moléculas, aunque no lo sean estrictamente en química. Estas moléculas producen tantas líneas en el espectro de una estrella tipo M que las líneas parecen fusionarse en enormes bandas que suprimen grandes trozos del espectro. En las estrellas tipo M, el óxido de titanio presenta un gran número de estas bandas en la luz visible, dominando enormes regiones del espectro.",
"alt_text": "Una línea entrecortada que aumenta a longitudes de onda más largas con grandes caídas anchas y algunas caídas más pronunciadas.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-m-type-star_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-m-type-star_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/d156Ob46Ih98/"
},
{
"diagram_label": "Stellar spectral types",
"diagram_slug": "Tt35DR10iI63",
"diagram_title": "Tipos espectrales estelares",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectros de siete estrellas ordenados por tipo espectral, desde las más calientes (tipo O) hasta las más frías (tipo M). El eje x muestra la longitud de onda de la luz y el eje y es una medida del flujo de luz recibida en esa longitud de onda. Cada espectro está normalizado (el flujo en cada longitud de onda se divide por el flujo máximo en ese espectro) y los espectros están desplazados entre sí a lo largo del eje y para facilitar la visualización del gráfico. El color de las líneas entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas estrellas más calientes tienen más flujo en el extremo azul del espectro y las estrellas más frías tienen más flujo en el extremo rojo. Sin embargo, la cantidad total de flujo que emite una estrella depende de su tamaño y temperatura. Debido a esto, una estrella caliente emitirá más luz roja que una estrella fría del mismo tamaño, incluso si la estrella fría emite casi toda su luz en luz roja, pero esto no es visible en este gráfico debido a la normalización mencionada anteriormente. Las caídas agudas y estrechas en los espectros son líneas de absorción causadas por átomos e iones en las atmósferas de las estrellas. La intensidad de una línea espectral depende de la temperatura de la atmósfera de la estrella. Tomemos como ejemplo la línea de hidrógeno a 656,5 nm. Todas las estrellas de este gráfico están formadas principalmente por hidrógeno, sin embargo, la línea de hidrógeno a 656,5 nm es débil en las estrellas más calientes y más frías, pero más fuerte en los tipos espectrales A y F. Esto se debe a que el hidrógeno absorbe más luz a 656,5 nm a las temperaturas de las atmósferas de las estrellas A y F que en las estrellas más calientes o más frías.\r\n\r\nLa estrella más fría aquí, la de tipo M, tiene bandas de absorción anchas en su espectro. Esto se debe a que esta estrella es lo suficientemente fría como para tener compuestos como el óxido de titanio en su atmósfera. Estos compuestos, a menudo llamados moléculas en astronomía, producen características de absorción espectral más amplias que los átomos o los iones.",
"alt_text": "Siete líneas. El pico de cada línea va de longitudes de onda cortas en la línea superior hasta longitudes de onda más largas en la línea inferior.",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-lines_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-lines_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/Tt35DR10iI63/"
},
{
"diagram_label": "Stellar spectral types - bands",
"diagram_slug": "W970mQ74LZ29",
"diagram_title": "Tipos espectrales estelares - bandas",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Espectros de siete estrellas ordenados por tipo espectral, desde las más calientes (tipo O) hasta las más frías (tipo M). El eje x muestra la longitud de onda de la luz, mientras que el brillo o la oscuridad en cada longitud de onda corresponde al flujo de luz recibido de la estrella en esa longitud de onda, teniendo las zonas más oscuras menos flujo y las más brillantes más. Cada espectro está normalizado (el flujo en cada longitud de onda se divide por el flujo máximo para ese espectro) de modo que el flujo máximo aparece con el mismo brillo en todos los espectros. El color trazado entre 400 nm y 700 nm corresponde aproximadamente al color en que el ojo humano vería la luz de esa longitud de onda. Por debajo de 400 nm y por encima de 700 nm, donde el ojo humano puede ver poca o ninguna luz, las líneas son de color azul y rojo, respectivamente.\r\n\r\nLas estrellas más calientes tienen más flujo en el extremo azul del espectro y las estrellas más frías tienen más flujo en el extremo rojo. Sin embargo, la cantidad total de flujo que emite una estrella depende de su tamaño y temperatura. Debido a esto, una estrella caliente emitirá más luz roja que una estrella fría del mismo tamaño, incluso si la estrella fría emite casi toda su luz en luz roja, pero esto no es visible en este gráfico debido a la normalización mencionada anteriormente. Las manchas oscuras y estrechas en los espectros son líneas de absorción causadas por átomos e iones en las atmósferas de las estrellas. La intensidad de una línea espectral depende de la temperatura de la atmósfera de la estrella. Tomemos como ejemplo la línea de hidrógeno a 656,5 nm. Todas las estrellas de este gráfico están formadas principalmente por hidrógeno, sin embargo, la línea de hidrógeno a 656,5 nm es débil en las estrellas más calientes y más frías, pero más fuerte en los tipos espectrales A y F. Esto se debe a que el hidrógeno absorbe más luz a 656,5 nm a las temperaturas de las atmósferas de las estrellas A y F que en las estrellas más calientes o más frías.\r\n\r\nLa estrella más fría aquí, la de tipo M, tiene bandas de absorción anchas en su espectro. Esto se debe a que esta estrella es lo suficientemente fría como para tener compuestos como el óxido de titanio en su atmósfera. Estos compuestos, a menudo llamados moléculas en astronomía, producen características de absorción espectral más amplias que los átomos o los iones.",
"alt_text": "Siete bandas con manchas brillantes y oscuras. La parte más brillante de la banda pasa del azul en la banda superior al rojo en la inferior",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-bands_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-bands_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/W970mQ74LZ29/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "إشعاع الجسم الأسود",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "منحنيات الإشعاع المنبعث من الأجسام السوداء ذات درجات الحرارة المختلفة. يُمثل المحور الأفقي (محور السينات) الطول الموجي، بينما يُمثل المحور العامودي (محور الصادات) كمية الطاقة المنبعثة كل ثانية بواسطة متر مربع واحد من سطح الجسم الأسود عند كل طول موجي. \r\nكلما كان الجسم أكثر سخونة، كان الطول الموجي أقصر والضوء الذي يصدره اكثر زرقة كلما انبعثت منه أقصى كمية من الطاقة. على الرغم من أن الجسم الأكثر برودة في هذا الرسم البياني يبلغ ذروته في الضوء الأحمر، إلا أن الأجسام الأخرى الأكثر سخونة تبعث جميعها ضوءاً أحمر أكثر من الجسم الأكثر برودة.",
"alt_text": "ثلاثة منحنيات تُبين الإشعاع على المحور الصادي والطول الموجي على المحور السيني. المنحنيات الأكثر برودة لها قمم اكثر احمراراً واقل ارتفاعاً.",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "إشعاع الجسم الأسود - كارثة الأشعة فوق البنفسجية",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "منحنيات الإشعاع المنبعث من الأجسام السوداء ذات درجات الحرارة المختلفة. يُمثل المحور الأفقي (محور السينات) الطول الموجي، بينما يُمثل المحور العامودي (محور الصادات) كمية الطاقة المنبعثة كل ثانية بواسطة متر مربع واحد من سطح الجسم الأسود عند كل طول موجي. \r\nكلما كان الجسم أكثر سخونة، كان الطول الموجي أقصر والضوء الذي يصدره اكثر زرقة كلما انبعثت منه أقصى كمية من الطاقة. على الرغم من أن الجسم الأكثر برودة في هذا الرسم البياني يبلغ ذروته في الضوء الأحمر، إلا أن الأجسام الأخرى الأكثر سخونة تبعث جميعها ضوءاً أحمر أكثر من الجسم الأكثر برودة. يوضح الخط المنقط الإشعاع المنبعث الذي تنبأت به النظرية الكلاسيكية قبل ميكانيكا الكم الحديثة. يميل هذا التنبؤ إلى اللانهاية عند الأطوال الموجية الأقصر لأي درجة حرارة للجسم الأسود أعلى من الصفر، وقد أُطلق عليها اسم \"كارثة الأشعة فوق البنفسجية\".",
"alt_text": "ثلاثة منحنيات تُبين الإشعاع على المحور الصادي والطول الموجي على المحور السيني. المنحنيات الأكثر برودة لها قمم اكثر احمراراً واقل ارتفاعاً.",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_ar_ouA60Ia.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_ar_KMF1AGF.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Spectrum of an O-type star",
"diagram_slug": "m5801x5SA50",
"diagram_title": "طيف لنجم من النوع O",
"glossary_terms": [
328,
382,
463
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "شكل يوضح طيف النجم HD 235673 وهو من النوع O، المحور السيني (الافقي) يمثل الطول الموجي بالنانومتر، بينما المحور الصادي ( العامودي) يمثل الفيض. يُظهر الجزء العلوي من المخطط نفس الطيف ولكن مع وجود بقع ساطعة للأطوال الموجية ذات الفيض العالي وبقع داكنة للأطوال الموجية ذات الفيض المنخفض. لون الخط بين 400 نانومتر و 700 نانومتر يتوافق تقريباً مع اللون الذي تراه العين البشرية للضوء بهذا الطول الموجي. أقل من 400 نانومتر وما فوق 700 نانومتر، حيث يمكن للعين البشرية أن ترى القليل من الضوء أو لا ترى أي ضوء، تكون الخطوط ملونة باللونين الأزرق والأحمر على التوالي. تُظهر الخطوط السوداء خطوط امتصاص طيفية ناتجة عن ذرات وأيونات العناصر المختلفة الموجودة في الغلاف الجوي للنجم. تمتص هذه الذرات والأيونات عند أطوال موجية محددة، مما يسبب خطوطاً حادة ومظلمة في الأطياف. وتعتمد مدى قوة هذه الخطوط على درجة حرارة الغلاف الجوي للنجم. يمكن لنجمين متكونين من نفس العناصر أن يكون لهما أطياف بمجموعات خطوط مختلفة تماماً إذا كانت درجات الحرارة في غلافهما الجوي مختلفة. اهم الخصائص الطيفية للنجوم من النوع O هي وجود عدد صغير من الخطوط الناتجة عن الهيليوم المتأين. تكون هذه الخطوط أقوى في النجوم من النوع O مقارنة بالنجوم الباردة. تظهر أيضاً خطوط من ذرات الهيليوم وذرات الهيدروجين في الطيف. الطيف له فيض أكثر في الطرف الأزرق مقارنة بالطرف الأحمر منه.",
"alt_text": "ينحدر الخط بسلاسة عند الأطوال الموجية الطويلة مع بعض الانخفاضات الحادة",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-o-type-star_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-o-type-star_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/m5801x5SA50/"
},
{
"diagram_label": "Spectrum of a B-type star",
"diagram_slug": "QF74Q764Tb95",
"diagram_title": "طيف لنجم من النوع B",
"glossary_terms": [
37,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "شكل يوضح طيف النجم HD258982 وهو من النوع B. يتوافق لون الخط الواقع بين 400 نانومتر و700 نانومتر تقريباً مع اللون الذي تراه العين البشرية من هذا الطول الموجي. تحت 400 نانومتر وفوق 700 نانومتر، حيث يمكن للعين البشرية أن ترى ضوءاً ضئيلاً أو لا ترى أي ضوء، تكون الخطوط ملونة باللونين الأزرق والأحمر على التوالي.\r\nتُظهر الخطوط السوداء خطوط الامتصاص الطيفي الناتجة عن ذرات وأيونات العناصر المختلفة في الغلاف الجوي للنجم. تمتص هذه الذرات والأيونات عند أطوال موجية محددة، مسببة خطوطاً حادة داكنة في الأطياف. وتعتمد قوة هذه الخطوط على درجة حرارة الغلاف الجوي للنجم. يمكن لنجمين متكونين من نفس العناصر أن يكون لهما أطياف بمجموعات خطوط مختلفة تماماً إذا كانت درجات الحرارة في غلافهما الجوي مختلفة. أما بالنسبة للنجوم من النوع B، فإن أهم الخطوط تنتج عن ذرات الهيليوم. وتكون هذه الخطوط أقوى في النجوم من النوع B وأضعف في الأنواع الأكثر حرارة والأكثر برودة. توجد أيضاً خطوط من ذرات الهايدروجين ولكنها ليست بقوة تلك الموجودة في النجوم الأبرد من النوع A.",
"alt_text": "ينحدر الخط بسلاسة عند الأطوال الموجية الطويلة مع بعض الانخفاضات الحادة",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-b-type-star_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-b-type-star_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/QF74Q764Tb95/"
},
{
"diagram_label": "Spectrum of an A-type star",
"diagram_slug": "2149RS77wy92",
"diagram_title": "طيف نجم من النوع A",
"glossary_terms": [
1,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "شكل يوضح طيف النجم BD-11 1212 وهو من النوع A. يتوافق لون الخط الواقع بين 400 نانومتر و700 نانومتر تقريباً مع اللون الذي تراه العين البشرية من هذا الطول الموجي. تحت 400 نانومتر وفوق 700 نانومتر، حيث يمكن للعين البشرية أن ترى ضوءاً ضئيلاً أو لا ترى أي ضوء، تكون الخطوط ملونة باللونين الأزرق والأحمر على التوالي.\r\nتُظهر الخطوط السوداء خطوط الامتصاص الطيفي الناتجة عن ذرات وأيونات العناصر المختلفة في الغلاف الجوي للنجم. تمتص هذه الذرات والأيونات عند أطوال موجية محددة، مسببة خطوطاً حادة داكنة في الأطياف. وتعتمد قوة هذه الخطوط على درجة حرارة الغلاف الجوي للنجم. يمكن لنجمين متكونين من نفس العناصر أن يكون لهما أطياف بمجموعات خطوط مختلفة تماماً إذا كانت درجات الحرارة في غلافهما الجوي مختلفة. تهيمن الخطوط الناتجة عن ذرات الهايدروجين على أطياف النجوم من النوع A وهي الأقوى في هذا النوع الطيفي.",
"alt_text": "يرتفع الخط بسلاسة ويصل الى ذروته عند حوالي 420 نانومتر ثم ينخفض عند الأطوال الموجية الأطول مع وجود بعض الانخفاضات العميقة نسبياً.",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-a-type-star_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-a-type-star_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/2149RS77wy92/"
},
{
"diagram_label": "Spectrum of an F-type star",
"diagram_slug": "zY580V14PE47",
"diagram_title": "طيف نجم من النوع F",
"glossary_terms": [
110,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "شكل يوضح طيف النجم 2MASS J22243289+4937443 وهو من النوع F. يتوافق لون الخط الواقع بين 400 نانومتر و700 نانومتر تقريباً مع اللون الذي تراه العين البشرية من هذا الطول الموجي. تحت 400 نانومتر وفوق 700 نانومتر، حيث يمكن للعين البشرية أن ترى ضوءاً ضئيلاً أو لا ترى أي ضوء، تكون الخطوط ملونة باللونين الأزرق والأحمر على التوالي.\r\nتُظهر الخطوط السوداء خطوط الامتصاص الطيفي الناتجة عن ذرات وأيونات العناصر المختلفة في الغلاف الجوي للنجم. تمتص هذه الذرات والأيونات عند أطوال موجية محددة، مسببة خطوطاً حادة داكنة في الأطياف. وتعتمد قوة هذه الخطوط على درجة حرارة الغلاف الجوي للنجم. يمكن لنجمين متكونين من نفس العناصر أن يكون لهما أطياف بمجموعات خطوط مختلفة تماماً إذا كانت درجات الحرارة في غلافهما الجوي مختلفة. لا تزال الخطوط الناتجة عن ذرات الهايدروجين والتي تعتبر الأقوى في النجوم من النوع A قوية نسبياً في النجوم من النوع F، لكن الخطوط الناتجة عن المعادن، وخاصة الكالسيوم المتأين تبدأ بأحتلال الصدارة (اي تكون هي الاقوى) في هذا النوع الطيفي.",
"alt_text": "يرتفع الخط بسلاسة نسبياً ويبلغ ذروته عند 430 نانومتر ثم ينخفض عند الاطوال الموجية الطويلة مع بعض الانخفاضات العميقة نسبياً.",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-f-type-star_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-f-type-star_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/zY580V14PE47/"
},
{
"diagram_label": "Spectrum of a G-type star",
"diagram_slug": "mX21es50Pj16",
"diagram_title": "طيف نجم من النوع G",
"glossary_terms": [
328,
382,
442
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "شكل يوضح طيف النجم UCAC4 700-069569 وهو من النوع G. يتوافق لون الخط الواقع بين 400 نانومتر و700 نانومتر تقريباً مع اللون الذي تراه العين البشرية من هذا الطول الموجي. تحت 400 نانومتر وفوق 700 نانومتر، حيث يمكن للعين البشرية أن ترى ضوءاً ضئيلاً أو لا ترى أي ضوء، تكون الخطوط ملونة باللونين الأزرق والأحمر على التوالي.\r\nتُظهر الخطوط السوداء خطوط الامتصاص الطيفي الناتجة عن ذرات وأيونات العناصر المختلفة في الغلاف الجوي للنجم. تمتص هذه الذرات والأيونات عند أطوال موجية محددة، مسببة خطوطاً حادة داكنة في الأطياف. وتعتمد قوة هذه الخطوط على درجة حرارة الغلاف الجوي للنجم. يمكن لنجمين متكونين من نفس العناصر أن يكون لهما أطياف بمجموعات خطوط مختلفة تماماً إذا كانت درجات الحرارة في غلافهما الجوي مختلفة. في النجوم من النوع G تكون الخطوط الناتجة من ذرات الهايدروجين أضعف من النجوم من النوع F بينما الخطوط الناتجة من الكالسيوم المتأين تكون أقوى. كما تبدأ تبرز الخطوط الناتجة من ذرات المعادن مثل ذرات الحديد والصوديوم والكالسيوم.",
"alt_text": "خط متعرج للغاية يبلغ ذروته في 470 نانومتر تقريباً ثم يبدأ بالانخفاض عند الاطوال الموجية الطويلة مع بعض الانخفاضات العميقة.",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-g-type-star_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-g-type-star_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/mX21es50Pj16/"
},
{
"diagram_label": "Spectrum of a K-type star",
"diagram_slug": "lH42QC364e69",
"diagram_title": "طيف نجم من النوع K",
"glossary_terms": [
168,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "شكل يوضح طيف النجم 2MASS J19554455+4754531 وهو من النوع K. يتوافق لون الخط الواقع بين 400 نانومتر و700 نانومتر تقريباً مع اللون الذي تراه العين البشرية من هذا الطول الموجي. تحت 400 نانومتر وفوق 700 نانومتر، حيث يمكن للعين البشرية أن ترى ضوءاً ضئيلاً أو لا ترى أي ضوء، تكون الخطوط ملونة باللونين الأزرق والأحمر على التوالي.\r\nتُظهر الخطوط السوداء خطوط الامتصاص الطيفي الناتجة عن ذرات وأيونات العناصر المختلفة في الغلاف الجوي للنجم. تمتص هذه الذرات والأيونات عند أطوال موجية محددة، مسببة خطوطاً حادة داكنة في الأطياف. وتعتمد قوة هذه الخطوط على درجة حرارة الغلاف الجوي للنجم. يمكن لنجمين متكونين من نفس العناصر أن يكون لهما أطياف بمجموعات خطوط مختلفة تماماً إذا كانت درجات الحرارة في غلافهما الجوي مختلفة. تهيمن ذرات المعادن مثل ذرات الحديد والصوديوم والكالسيوم على أطياف النجوم من النوع K. هناك العديد من الخطوط الناتجة من ذرات المعادن ، وهي كثيرة جدا لدرجة انه لا يمكن تمييزها بشكل فردي ، بحيث يكون للطيف مظهر متقطع وخشن. خطوط ذرات الهايدروجين وأيونات الكالسيوم أضعف بكثير من النجوم الأكثر حرارة من النوع G.",
"alt_text": "خط متعرج يبلغ ذروته عند 580 نانومتر تقريباً ثم يبدأ بالانخفاض عند الاطوال الموجية الاطول مع بعض الانخفاضات العميقة.",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-k-type-star_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-k-type-star_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/lH42QC364e69/"
},
{
"diagram_label": "Spectrum of an M-type star",
"diagram_slug": "d156Ob46Ih98",
"diagram_title": "طيف نجم من النوع M",
"glossary_terms": [
328,
382,
453
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "شكل يوضح طيف النجم 2MASS J15581272+8457104 وهو من النوع M. يتوافق لون الخط الواقع بين 400 نانومتر و700 نانومتر تقريباً مع اللون الذي تراه العين البشرية من هذا الطول الموجي. تحت 400 نانومتر وفوق 700 نانومتر، حيث يمكن للعين البشرية أن ترى ضوءاً ضئيلاً أو لا ترى أي ضوء، تكون الخطوط ملونة باللونين الأزرق والأحمر على التوالي.\r\nتُظهر الخطوط السوداء خطوط الامتصاص الطيفي الناتجة عن ذرات وأيونات العناصر المختلفة في الغلاف الجوي للنجم. تمتص هذه الذرات والأيونات عند أطوال موجية محددة، مسببة خطوطاً حادة داكنة في الأطياف. وتعتمد قوة هذه الخطوط على درجة حرارة الغلاف الجوي للنجم. يمكن لنجمين متكونين من نفس العناصر أن يكون لهما أطياف بمجموعات خطوط مختلفة تماماً إذا كانت درجات الحرارة في غلافهما الجوي مختلفة. تكون الأغلفة الجوية للنجوم من النوع M باردة بما يكفي لتكوين بعض المركبات الكيميائية. وغالباً ما يُشار إليها بالجزيئات في علم الفلك، حتى لو لم تكن جزيئات بالمعنى الكيميائي الدقيق. وتنتج هذه الجزيئات العديد من الخطوط في طيف نجم من النوع M بحيث تبدو الخطوط وكأنها تندمج معاً في نطاقات ضخمة تزيل أجزاء كبيرة من الطيف. في النجوم من النوع M، يحتوي أوكسيد التيتانيوم على عدد كبير من هذه النطاقات في الضوء المرئي، مهيمناً على مناطق ضخمة من الطيف.",
"alt_text": "خط متقطع يتزايد عند الأطوال الموجية الأطول مع انخفاضات كبيرة واسعة وبعض الانخفاضات الحادة.",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-m-type-star_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-m-type-star_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/d156Ob46Ih98/"
},
{
"diagram_label": "Stellar spectral types",
"diagram_slug": "Tt35DR10iI63",
"diagram_title": "الأنواع الطيفية النجمية",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "أطياف سبعة نجوم مرتبة حسب النوع الطيفي بدءاً من الأكثر سخونة (النوع O) في الأعلى إلى الأكثر برودة (النوع M في الأسفل). يمثل المحور الأفقي (السيني) الطول الموجي للضوء بينما المحور العامودي (الصادي) يمثل مقياس فيض الضوء المستلم عند هذا الطول الموجي. يتم تطبيع كل طيف (يتم قسمة الفيض عند كل طول موجي على الحد الأقصى للفيض في هذا الطيف) ثم يتم إزاحة الأطياف عن بعضها البعض على طول المحور العامودي (الصادي) لتسهيل عرض الرسم البياني. يتطابق لون الخطوط بين 400 نانومتر و700 نانومتر تقريباً مع اللون الذي تراه العين البشرية من هذا الطول الموجي. أقل من 400 نانومتر وأعلى من 700 نانومتر، حيث يمكن للعين البشرية أن ترى ضوءاً ضئيلاً أو لا ترى أي ضوء، فإن الخطوط ملونة باللونين الأزرق والأحمر على التوالي.\r\nيكون معظم الفيض الضوئي للنجوم الأكثر حرارة في الطرف الأكثر زرقة من الطيف، بينما يكون معظم الفيض الضوئي للنجوم الأكثر برودة في الطرف الأكثر احمراراً منه. لكن كمية الفيض الكلية التي يبعثها النجم تعتمد على حجمه ودرجة حرارته. ونتيجة لذلك، يبعث النجم الساخن ضوءاً أحمر أكثر من النجم البارد من نفس الحجم حتى لو كان النجم البارد يبعث كل ضوءه تقريباً في في مدى الضوء الأحمر، لكن هذا لايظهر في هذا الرسم البياني بسبب التطبيع المذكور أعلاه. إن الانخفاضات الحادة والضيقة في الأطياف هي خطوط امتصاص ناتجة عن الذرات والأيونات في الغلاف الجوي للنجوم. تعتمد قوة الخط الطيفي على درجة حرارة الغلاف الجوي للنجم. لنأخذ خط الهايدروجين عند 656.5 نانومتر كمثال. جميع خطوط النجوم في هذا الرسم البياني ناتجة من الهايدروجين بشكل رئيسي، لكن خط الهايدروجين عند 656.5 نانومتر يكون ضعيفاً في النجوم الأكثر حرارة والأكثر برودة ولكنه أقوى في النوعين الطيفيين A و F. وذلك لأن الهايدروجين يمتص ضوءاً عند 656.5 نانومتر عند درجة حرارة الغلاف الجوي للنجوم A و F أكثر من النجوم الأكثر حرارة أو برودة.\r\nالنجم الأكثر برودة هنا هو النجم من النوع M، لديه نطاقات امتصاص واسعة في أطيافه. هذا لأن هذا النجم بارد بما يكفي ليكون لديه مركبات مثل أوكسيد التيتانيوم في غلافه الجوي. وتنتج هذه المركبات، التي غالباً ما تسمى جزيئات في علم الفلك، سمات امتصاص طيفي أوسع من الذرات أو الأيونات.",
"alt_text": "سبعة خطوط. تنتقل قمة كل خط من الأطوال الموجية القصيرة للخط العلوي إلى الأطوال الموجية الأطول للخط السفلي.",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
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"license": "CC-BY-4.0",
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"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-lines_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-lines_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/Tt35DR10iI63/"
},
{
"diagram_label": "Stellar spectral types - bands",
"diagram_slug": "W970mQ74LZ29",
"diagram_title": "الأنواع الطيفية النجمية - النطاقات",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "أطياف سبعة نجوم مرتبة حسب النوع الطيفي بدءاً من الأكثر سخونة (النوع O) في الأعلى إلى الأكثر برودة (النوع M في الأسفل). يمثل المحور الأفقي (السيني) الطول الموجي للضوء بينما المحور العامودي (الصادي) يمثل مقياس فيض الضوء المستلم عند هذا الطول الموجي. يتم تطبيع كل طيف (يتم قسمة الفيض عند كل طول موجي على الحد الأقصى للفيض في هذا الطيف) ثم يتم إزاحة الأطياف عن بعضها البعض على طول المحور العامودي (الصادي) لتسهيل عرض الرسم البياني. يتطابق لون الخطوط بين 400 نانومتر و700 نانومتر تقريباً مع اللون الذي تراه العين البشرية من هذا الطول الموجي. أقل من 400 نانومتر وأعلى من 700 نانومتر، حيث يمكن للعين البشرية أن ترى ضوءاً ضئيلاً أو لا ترى أي ضوء، فإن الخطوط ملونة باللونين الأزرق والأحمر على التوالي.\r\nيكون معظم الفيض الضوئي للنجوم الأكثر حرارة في الطرف الأكثر زرقة من الطيف، بينما يكون معظم الفيض الضوئي للنجوم الأكثر برودة في الطرف الأكثر احمراراً منه. لكن كمية الفيض الكلية التي يبعثها النجم تعتمد على حجمه ودرجة حرارته. ونتيجة لذلك، يبعث النجم الساخن ضوءاً أحمر أكثر من النجم البارد من نفس الحجم حتى لو كان النجم البارد يبعث كل ضوءه تقريباً في في مدى الضوء الأحمر، لكن هذا لايظهر في هذا الرسم البياني بسبب التطبيع المذكور أعلاه. إن الانخفاضات الحادة والضيقة في الأطياف هي خطوط امتصاص ناتجة عن الذرات والأيونات في الغلاف الجوي للنجوم. تعتمد قوة الخط الطيفي على درجة حرارة الغلاف الجوي للنجم. لنأخذ خط الهايدروجين عند 656.5 نانومتر كمثال. جميع خطوط النجوم في هذا الرسم البياني ناتجة من الهايدروجين بشكل رئيسي، لكن خط الهايدروجين عند 656.5 نانومتر يكون ضعيفاً في النجوم الأكثر حرارة والأكثر برودة ولكنه أقوى في النوعين الطيفيين A و F. وذلك لأن الهايدروجين يمتص ضوءاً عند 656.5 نانومتر عند درجة حرارة الغلاف الجوي للنجوم A و F أكثر من النجوم الأكثر حرارة أو برودة.\r\nالنجم الأكثر برودة هنا هو النجم من النوع M، لديه نطاقات امتصاص واسعة في أطيافه. هذا لأن هذا النجم بارد بما يكفي ليكون لديه مركبات مثل أوكسيد التيتانيوم في غلافه الجوي. وتنتج هذه المركبات، التي غالباً ما تسمى جزيئات في علم الفلك، سمات امتصاص طيفي أوسع من الذرات أو الأيونات.",
"alt_text": "سبعة نطاقات ذات بقع مضيئة وداكنة. ينتقل الجزء الأكثر سطوعاً من النطاق من الأزرق في النطاق العلوي إلى الأحمر في النطاق الأسفل",
"credit_text": "مكتب الاتحاد الفلكي الدولي للتعليم / مسح سلووان الرقمي للسماء/ نايال ديكون",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-bands_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-bands_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/W970mQ74LZ29/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "कृष्णिका (ब्लॅकबॉडी) प्रारण",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "वेगवेगळ्या तापमानाच्या ब्लॅकबॉडीजमधून उत्सर्जित रेडिएशनचे वक्र. x-अक्ष तरंगलांबी दर्शवतो आणि y-अक्ष प्रत्येक तरंगलांबीवर त्या ब्लॅकबॉडीच्या पृष्ठभागाच्या चौरस मीटरने प्रत्येक सेकंदाला उत्सर्जित होणारी ऊर्जा दर्शवितो. शरीर जितके गरम असेल तितकी तरंगलांबी कमी आणि निळा प्रकाश जास्तीत जास्त ऊर्जा उत्सर्जित करते. या प्लॉटमधील सर्वात थंड शरीर लाल प्रकाशात शिखरावर असूनही, इतर गरम शरीरे सर्वांत थंड शरीरापेक्षा जास्त लाल प्रकाश उत्सर्जित करतात.",
"alt_text": "y-अक्षावर रेडिएशन आणि x-अक्षावर तरंगलांबी असलेले तीन वक्र. थंड वक्रांमध्ये लालसर आणि खालची शिखरे असतात.",
"credit_text": "अंतर्राष्ट्रीय खगोलीय संघ खगोलशास्त्र शिक्षण कार्यालय (IAU-OAE) - नियाल डिकॉन",
"credit_url": null,
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"language_code": "mr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_mr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_mr.pdf",
"diagram_url": "https://astro4edu.org/mr/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "कृष्णिका प्रारण अतिनील आपत्ती",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "वेगवेगळ्या तापमानाच्या ब्लॅकबॉडीजमधून उत्सर्जित रेडिएशनचे वक्र. x-अक्ष तरंगलांबी दर्शवतो आणि y-अक्ष प्रत्येक तरंगलांबीवर त्या ब्लॅकबॉडीच्या पृष्ठभागाच्या चौरस मीटरने प्रत्येक सेकंदाला उत्सर्जित होणारी ऊर्जा दर्शवितो. शरीर जितके गरम असेल तितकी तरंगलांबी कमी आणि निळा प्रकाश जास्तीत जास्त ऊर्जा उत्सर्जित करते. या प्लॉटमधील सर्वात थंड शरीर लाल प्रकाशात शिखरावर असूनही, इतर गरम शरीरे सर्वांत थंड शरीरापेक्षा जास्त लाल प्रकाश उत्सर्जित करतात. ठिपके असलेली रेषा आधुनिक क्वांटम मेकॅनिक्सच्या अगोदर शास्त्रीय सिद्धांतानुसार उत्सर्जित रेडिएशन दर्शवते. ही भविष्यवाणी शून्यापेक्षा जास्त ब्लॅकबॉडी तापमानासाठी कमी तरंगलांबीमध्ये अनंततेकडे झुकते आणि त्याला 'अतिनील (अल्ट्राव्हायोलेट) आपत्ती' असे नाव देण्यात आले.",
"alt_text": "y-अक्षावर रेडिएशन आणि x-अक्षावर तरंगलांबी असलेले तीन वक्र. थंड वक्रांमध्ये लालसर आणि खालची शिखरे असतात.",
"credit_text": "अंतर्राष्ट्रीय खगोलीय संघ खगोलशास्त्र शिक्षण कार्यालय (IAU-OAE) - नियाल डिकॉन",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "mr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_mr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_mr.pdf",
"diagram_url": "https://astro4edu.org/mr/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "黑體輻射",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "不同溫度黑體的輻射麯綫。x 軸錶示波長，y 軸錶示黑體錶麵每平方米在每個波長下每秒發射的能量。\r\n\r\n溫度越高的物體，波長越短，發齣的最大能量光也越藍。盡管圖中最冷的天體發齣的紅光達到峰值，但其他較熱的天體發齣的紅光都比最冷的天體多。",
"alt_text": "三條麯綫，Y 軸為輻射，X 軸為波長。較冷的麯綫峰值較紅和較低",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "黑体辐射",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "不同温度黑体的辐射曲线。x 轴表示波长，y 轴表示黑体表面每平方米在每个波长下每秒发射的能量。\r\n\r\n温度越高的物体，波长越短，发出的最大能量光也越蓝。尽管图中最冷的天体发出的红光达到峰值，但其他较热的天体发出的红光都比最冷的天体多。",
"alt_text": "三条曲线，Y 轴为辐射，X 轴为波长。较冷的曲线峰值较红和较低",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "黑體輻射--紫外綫災難",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "不同溫度黑體的輻射麯綫。x 軸錶示波長，y 軸錶示黑體錶麵每平方米在每個波長下每秒發射的能量。\r\n\r\n溫度越高的物體，波長越短，發齣的最大能量光也越藍。盡管圖中最冷的天體發齣的紅光達到峰值，但其他較熱的天體發齣的紅光都比最冷的天體多。\r\n\r\n虛綫顯示的是現代量子力學之前的經典理論所預測的輻射量。對於任何溫度高於零的黑體，這一預測在較短波長處都趨於無窮大，被稱為 \"紫外綫災難\"。",
"alt_text": "三條麯綫，Y 軸為輻射，X 軸為波長。較冷的麯綫峰值較紅和較低",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "黑体辐射--紫外线灾难",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
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"caption": "不同温度黑体的辐射曲线。x 轴表示波长，y 轴表示黑体表面每平方米在每个波长下每秒发射的能量。\r\n\r\n温度越高的物体，波长越短，发出的最大能量光也越蓝。尽管图中最冷的天体发出的红光达到峰值，但其他较热的天体发出的红光都比最冷的天体多。\r\n\r\n虚线显示的是现代量子力学之前的经典理论所预测的辐射量。对于任何温度高于零的黑体，这一预测在较短波长处都趋于无穷大，被称为 \"紫外线灾难\"。",
"alt_text": "三条曲线，Y 轴为辐射，X 轴为波长。较冷的曲线峰值较红和较低",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Spectrum of an O-type star",
"diagram_slug": "m5801x5SA50",
"diagram_title": "一顆 O 型恒星的光譜",
"glossary_terms": [
328,
382,
463
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "O 型恒星 HD 235673 的光譜，X 軸為波長（納米），Y 軸為通量。圖的上半部分顯示瞭相同的光譜，但高通量的波長為亮斑，低通量的波長為暗斑。400 納米到 700 納米之間的綫條顔色與人眼看到的該波長光的顔色基本一緻。在 400 納米以下和 700 納米以上，人眼幾乎看不到光，這兩條綫的顔色分彆為藍色和紅色。\r\n\r\n黑綫錶示恒星大氣中不同元素的原子和離子造成的光譜吸收綫。這些原子和離子會吸收特定波長的光，從而在光譜中形成尖銳的暗綫。這些綫條的強度取決於恒星大氣層的溫度。如果兩顆恒星的大氣層溫度不同，那麼由相同元素混閤而成的兩顆恒星的光譜中可能會齣現大相徑庭的光譜綫。對於 O 型恒星來說，最重要的特徵是由電離氦引起的少量譜綫。O 型恒星中的這些譜綫比冷態恒星中的譜綫更強。氦原子和氫原子的譜綫也齣現在光譜中。光譜的藍色端比紅色端有更多的通量。",
"alt_text": "一條平滑的綫條，在較長的波長上呈下降趨勢，並伴有一些急劇下降。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-o-type-star_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-o-type-star_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/m5801x5SA50/"
},
{
"diagram_label": "Spectrum of an O-type star",
"diagram_slug": "m5801x5SA50",
"diagram_title": "一颗 O 型恒星的光谱",
"glossary_terms": [
328,
382,
463
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
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"caption": "O 型恒星 HD 235673 的光谱，X 轴为波长（纳米），Y 轴为通量。图的上半部分显示了相同的光谱，但高通量的波长为亮斑，低通量的波长为暗斑。400 纳米到 700 纳米之间的线条颜色与人眼看到的该波长光的颜色基本一致。在 400 纳米以下和 700 纳米以上，人眼几乎看不到光，这两条线的颜色分别为蓝色和红色。\r\n\r\n黑线表示恒星大气中不同元素的原子和离子造成的光谱吸收线。这些原子和离子会吸收特定波长的光，从而在光谱中形成尖锐的暗线。这些线条的强度取决于恒星大气层的温度。如果两颗恒星的大气层温度不同，那么由相同元素混合而成的两颗恒星的光谱中可能会出现大相径庭的光谱线。对于 O 型恒星来说，最重要的特征是由电离氦引起的少量谱线。O 型恒星中的这些谱线比冷态恒星中的谱线更强。氦原子和氢原子的谱线也出现在光谱中。光谱的蓝色端比红色端有更多的通量。",
"alt_text": "一条平滑的线条，在较长的波长上呈下降趋势，并伴有一些急剧下降。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
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"license": "CC-BY-4.0",
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"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-o-type-star_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-o-type-star_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/m5801x5SA50/"
},
{
"diagram_label": "Spectrum of a B-type star",
"diagram_slug": "QF74Q764Tb95",
"diagram_title": "一顆 B 型恒星的光譜",
"glossary_terms": [
37,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "B 型恒星 HD 258982 的光譜。波長在 400 納米到 700 納米之間的光譜綫的顔色大緻與人眼看到的該波長光綫的顔色一緻。波長低於 400 納米和高於 700 納米時，人眼幾乎看不到光，光譜綫的顔色分彆為藍色和紅色。\r\n\r\n黑綫錶示恒星大氣中不同元素的原子和離子造成的光譜吸收綫。這些原子和離子會吸收特定波長的光，從而在光譜中形成尖銳的暗綫。這些綫條的強度取決於恒星大氣層的溫度。如果兩顆恒星的大氣層溫度不同，那麼由相同元素混閤而成的兩顆恒星的光譜中可能會齣現大相徑庭的光譜綫。對於 B 型恒星來說，最重要的譜綫是由氦原子産生的。這些譜綫在 B 型恒星中最強，在較熱和較冷的類型中較弱。氫原子産生的譜綫也存在，但不如在較冷的 A 型恒星中那麼強。",
"alt_text": "一條平滑的綫條，在較長的波長上呈下降趨勢，並伴有一些急劇下降。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
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"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-b-type-star_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-b-type-star_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/QF74Q764Tb95/"
},
{
"diagram_label": "Spectrum of a B-type star",
"diagram_slug": "QF74Q764Tb95",
"diagram_title": "一颗 B 型恒星的光谱",
"glossary_terms": [
37,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "B 型恒星 HD 258982 的光谱。波长在 400 纳米到 700 纳米之间的光谱线的颜色大致与人眼看到的该波长光线的颜色一致。波长低于 400 纳米和高于 700 纳米时，人眼几乎看不到光，光谱线的颜色分别为蓝色和红色。\r\n\r\n黑线表示恒星大气中不同元素的原子和离子造成的光谱吸收线。这些原子和离子会吸收特定波长的光，从而在光谱中形成尖锐的暗线。这些线条的强度取决于恒星大气层的温度。如果两颗恒星的大气层温度不同，那么由相同元素混合而成的两颗恒星的光谱中可能会出现大相径庭的光谱线。对于 B 型恒星来说，最重要的谱线是由氦原子产生的。这些谱线在 B 型恒星中最强，在较热和较冷的类型中较弱。氢原子产生的谱线也存在，但不如在较冷的 A 型恒星中那么强。",
"alt_text": "一条平滑的线条，在较长的波长上呈下降趋势，并伴有一些急剧下降。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-b-type-star_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-b-type-star_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/QF74Q764Tb95/"
},
{
"diagram_label": "Spectrum of an A-type star",
"diagram_slug": "2149RS77wy92",
"diagram_title": "A 型恒星的光譜",
"glossary_terms": [
1,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "A 型恒星 BD-11 1212 的光譜。波長在 400 納米到 700 納米之間的光譜綫的顔色與人眼看到的該波長光綫的顔色大緻對應。在 400 納米以下和 700 納米以上，人眼幾乎看不到光，光譜綫分彆被染成藍色和紅色。\r\n\r\n黑綫錶示恒星大氣中不同元素的原子和離子造成的光譜吸收綫。這些原子和離子會吸收特定波長的光，從而在光譜中形成尖銳的暗綫。這些綫條的強度取決於恒星大氣層的溫度。如果兩顆恒星的大氣層溫度不同，那麼由相同元素混閤而成的兩顆恒星的光譜中可能會齣現截然不同的光譜綫。來自氫原子的光譜綫在 A 型恒星的光譜中占主導地位，並且在這種光譜類型中最強。",
"alt_text": "一條平滑的綫，在 420 納米波長處達到峰值，然後在較長的波長處下降，有幾個相當寬的凹點。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-a-type-star_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-a-type-star_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/2149RS77wy92/"
},
{
"diagram_label": "Spectrum of an A-type star",
"diagram_slug": "2149RS77wy92",
"diagram_title": "A 型恒星的光谱",
"glossary_terms": [
1,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "A 型恒星 BD-11 1212 的光谱。波长在 400 纳米到 700 纳米之间的光谱线的颜色与人眼看到的该波长光线的颜色大致对应。在 400 纳米以下和 700 纳米以上，人眼几乎看不到光，光谱线分别被染成蓝色和红色。\r\n\r\n黑线表示恒星大气中不同元素的原子和离子造成的光谱吸收线。这些原子和离子会吸收特定波长的光，从而在光谱中形成尖锐的暗线。这些线条的强度取决于恒星大气层的温度。如果两颗恒星的大气层温度不同，那么由相同元素混合而成的两颗恒星的光谱中可能会出现截然不同的光谱线。来自氢原子的光谱线在 A 型恒星的光谱中占主导地位，并且在这种光谱类型中最强。",
"alt_text": "一条平滑的线，在 420 纳米波长处达到峰值，然后在较长的波长处下降，有几个相当宽的凹点。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-a-type-star_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-a-type-star_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/2149RS77wy92/"
},
{
"diagram_label": "Spectrum of an F-type star",
"diagram_slug": "zY580V14PE47",
"diagram_title": "一顆 F 型恒星的光譜",
"glossary_terms": [
110,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "F 型恒星 2MASS J22243289+4937443 的光譜。波長在 400 納米到 700 納米之間的光譜綫的顔色大緻與人眼看到的該波長光綫的顔色一緻。波長低於 400 納米和高於 700 納米時，人眼幾乎看不到光，這兩條光譜綫分彆被染成藍色和紅色。\r\n\r\n黑綫錶示恒星大氣中不同元素的原子和離子造成的光譜吸收綫。這些原子和離子會吸收特定波長的光，從而在光譜中形成尖銳的暗綫。這些綫條的強度取決於恒星大氣層的溫度。如果兩顆恒星的大氣層溫度不同，那麼由相同元素混閤而成的兩顆恒星的光譜中可能會齣現截然不同的光譜綫。在 A 型恒星中最強的氫原子譜綫在 F 型恒星中仍然相對較強，但金屬（尤其是電離鈣）譜綫在這一光譜類型開始變得較強。",
"alt_text": "一條相對平滑的綫，在大約 430 納米波長處達到峰值，然後在較長的波長處下降，並有幾個相當寬的凹點。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
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"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-f-type-star_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-f-type-star_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/zY580V14PE47/"
},
{
"diagram_label": "Spectrum of an F-type star",
"diagram_slug": "zY580V14PE47",
"diagram_title": "一颗 F 型恒星的光谱",
"glossary_terms": [
110,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "F 型恒星 2MASS J22243289+4937443 的光谱。波长在 400 纳米到 700 纳米之间的光谱线的颜色大致与人眼看到的该波长光线的颜色一致。波长低于 400 纳米和高于 700 纳米时，人眼几乎看不到光，这两条光谱线分别被染成蓝色和红色。\r\n\r\n黑线表示恒星大气中不同元素的原子和离子造成的光谱吸收线。这些原子和离子会吸收特定波长的光，从而在光谱中形成尖锐的暗线。这些线条的强度取决于恒星大气层的温度。如果两颗恒星的大气层温度不同，那么由相同元素混合而成的两颗恒星的光谱中可能会出现截然不同的光谱线。在 A 型恒星中最强的氢原子谱线在 F 型恒星中仍然相对较强，但金属（尤其是电离钙）谱线在这一光谱类型开始变得较强。",
"alt_text": "一条相对平滑的线，在大约 430 纳米波长处达到峰值，然后在较长的波长处下降，并有几个相当宽的凹点。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
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"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-f-type-star_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-f-type-star_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/zY580V14PE47/"
},
{
"diagram_label": "Spectrum of a G-type star",
"diagram_slug": "mX21es50Pj16",
"diagram_title": "一顆 G 型恒星的光譜",
"glossary_terms": [
328,
382,
442
],
"categories": [
"Stars"
],
"category_ids": [
2
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"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "G 型恒星 UCAC4 700-069569 的光譜。波長在 400 納米到 700 納米之間的光譜綫的顔色大緻與人眼看到的該波長光綫的顔色一緻。在 400 納米以下和 700 納米以上，人眼幾乎看不到光，光譜綫分彆被染成藍色和紅色。\r\n\r\n黑綫錶示恒星大氣中不同元素的原子和離子造成的光譜吸收綫。這些原子和離子會吸收特定波長的光，從而在光譜中形成尖銳的暗綫。這些綫條的強度取決於恒星大氣層的溫度。如果兩顆恒星的大氣層溫度不同，那麼由相同元素混閤而成的兩顆恒星的光譜中可能會齣現截然不同的光譜綫。在 G 型恒星中，氫原子的光譜綫比 F 型恒星弱，而電離鈣的光譜綫則比 F 型恒星強。鐵、鈉和鈣等金屬原子的譜綫也開始變得突齣。",
"alt_text": "一條波長約為 470 納米的崎嶇綫條達到峰值，然後在較長的波長上逐漸減弱，並有幾處較深的凹陷。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-g-type-star_zh-hans_yENAsxK.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-g-type-star_zh-hans_1UqaNPO.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/mX21es50Pj16/"
},
{
"diagram_label": "Spectrum of a G-type star",
"diagram_slug": "mX21es50Pj16",
"diagram_title": "一颗 G 型恒星的光谱",
"glossary_terms": [
328,
382,
442
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "G 型恒星 UCAC4 700-069569 的光谱。波长在 400 纳米到 700 纳米之间的光谱线的颜色大致与人眼看到的该波长光线的颜色一致。在 400 纳米以下和 700 纳米以上，人眼几乎看不到光，光谱线分别被染成蓝色和红色。\r\n\r\n黑线表示恒星大气中不同元素的原子和离子造成的光谱吸收线。这些原子和离子会吸收特定波长的光，从而在光谱中形成尖锐的暗线。这些线条的强度取决于恒星大气层的温度。如果两颗恒星的大气层温度不同，那么由相同元素混合而成的两颗恒星的光谱中可能会出现截然不同的光谱线。在 G 型恒星中，氢原子的光谱线比 F 型恒星弱，而电离钙的光谱线则比 F 型恒星强。铁、钠和钙等金属原子的谱线也开始变得突出。",
"alt_text": "一条波长约为 470 纳米的崎岖线条达到峰值，然后在较长的波长上逐渐减弱，并有几处较深的凹陷。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-g-type-star_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-g-type-star_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/mX21es50Pj16/"
},
{
"diagram_label": "Spectrum of a K-type star",
"diagram_slug": "lH42QC364e69",
"diagram_title": "一顆 K 型恒星的光譜",
"glossary_terms": [
168,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "K 型恒星 2MASS J19554455+4754531 的光譜。波長在 400 納米到 700 納米之間的光譜綫的顔色大緻與人眼看到的該波長光綫的顔色一緻。波長低於 400 納米和高於 700 納米時，人眼幾乎看不到光，光譜綫分彆被染成藍色和紅色。\r\n\r\n黑綫錶示恒星大氣中不同元素的原子和離子造成的光譜吸收綫。這些原子和離子會吸收特定波長的光，從而在光譜中形成尖銳的暗綫。這些綫條的強度取決於恒星大氣層的溫度。如果兩顆恒星的大氣層溫度不同，那麼由相同元素混閤而成的兩顆恒星的光譜中可能會齣現大相徑庭的綫條。K 型恒星的光譜主要由鐵、鈉和鈣等金屬原子構成。金屬原子的譜綫非常多，多到無法逐一標齣，以至於光譜看起來波瀾不驚、參差不齊。氫原子和鈣離子的譜綫比更熱的 G 型恒星要弱得多。",
"alt_text": "一條波長約為 580 納米的鋸齒狀綫條達到峰值，然後在較長的波長上逐漸減弱，並有一些較深的凹陷。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-k-type-star_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-k-type-star_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/lH42QC364e69/"
},
{
"diagram_label": "Spectrum of a K-type star",
"diagram_slug": "lH42QC364e69",
"diagram_title": "一颗 K 型恒星的光谱",
"glossary_terms": [
168,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "K 型恒星 2MASS J19554455+4754531 的光谱。波长在 400 纳米到 700 纳米之间的光谱线的颜色大致与人眼看到的该波长光线的颜色一致。波长低于 400 纳米和高于 700 纳米时，人眼几乎看不到光，光谱线分别被染成蓝色和红色。\r\n\r\n黑线表示恒星大气中不同元素的原子和离子造成的光谱吸收线。这些原子和离子会吸收特定波长的光，从而在光谱中形成尖锐的暗线。这些线条的强度取决于恒星大气层的温度。如果两颗恒星的大气层温度不同，那么由相同元素混合而成的两颗恒星的光谱中可能会出现大相径庭的线条。K 型恒星的光谱主要由铁、钠和钙等金属原子构成。金属原子的谱线非常多，多到无法逐一标出，以至于光谱看起来波澜不惊、参差不齐。氢原子和钙离子的谱线比更热的 G 型恒星要弱得多。",
"alt_text": "一条波长约为 580 纳米的锯齿状线条达到峰值，然后在较长的波长上逐渐减弱，并有一些较深的凹陷。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-a-k-type-star_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-a-k-type-star_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/lH42QC364e69/"
},
{
"diagram_label": "Spectrum of an M-type star",
"diagram_slug": "d156Ob46Ih98",
"diagram_title": "一顆 M 型恒星的光譜",
"glossary_terms": [
328,
382,
453
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "M 型恒星 2MASS J15581272+8457104 的光譜。波長在 400 納米到 700 納米之間的光譜綫的顔色大緻與人眼看到的該波長光綫的顔色一緻。波長低於 400 納米和高於 700 納米時，人眼幾乎看不到光，這兩條綫分彆被染成藍色和紅色。\r\n\r\n黑綫顯示的是恒星大氣中不同元素的原子、離子和分子造成的光譜吸收綫。這些原子、離子和分子會吸收特定波長的光綫，從而在光譜中形成尖銳的暗綫。這些綫條的強度取決於恒星大氣層的溫度。如果兩顆恒星的大氣層溫度不同，那麼由相同元素混閤而成的兩顆恒星的光譜中可能會齣現截然不同的光譜綫。M 型恒星的大氣層足夠冷，可以形成一些化閤物。這些化閤物通常在天文學中被稱為分子，盡管它們在化學中並不是嚴格意義上的分子。這些分子會在 M 型恒星的光譜中産生如此之多的譜綫，以至於這些譜綫看起來會閤並成巨大的條帶，從而從光譜中去除一大塊。在 M 型恒星中，氧化鈦在可見光中有大量這樣的波段，占據瞭光譜的大部分區域。",
"alt_text": "波長較長的波浪綫，波幅較大，有幾個較尖銳的波峰。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-m-type-star_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-m-type-star_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/d156Ob46Ih98/"
},
{
"diagram_label": "Spectrum of an M-type star",
"diagram_slug": "d156Ob46Ih98",
"diagram_title": "一颗 M 型恒星的光谱",
"glossary_terms": [
328,
382,
453
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "M 型恒星 2MASS J15581272+8457104 的光谱。波长在 400 纳米到 700 纳米之间的光谱线的颜色大致与人眼看到的该波长光线的颜色一致。波长低于 400 纳米和高于 700 纳米时，人眼几乎看不到光，这两条线分别被染成蓝色和红色。\r\n\r\n黑线显示的是恒星大气中不同元素的原子、离子和分子造成的光谱吸收线。这些原子、离子和分子会吸收特定波长的光线，从而在光谱中形成尖锐的暗线。这些线条的强度取决于恒星大气层的温度。如果两颗恒星的大气层温度不同，那么由相同元素混合而成的两颗恒星的光谱中可能会出现截然不同的光谱线。M 型恒星的大气层足够冷，可以形成一些化合物。这些化合物通常在天文学中被称为分子，尽管它们在化学中并不是严格意义上的分子。这些分子会在 M 型恒星的光谱中产生如此之多的谱线，以至于这些谱线看起来会合并成巨大的条带，从而从光谱中去除一大块。在 M 型恒星中，氧化钛在可见光中有大量这样的波段，占据了光谱的大部分区域。",
"alt_text": "波长较长的波浪线，波幅较大，有几个较尖锐的波峰。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectrum-of-an-m-type-star_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectrum-of-an-m-type-star_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/d156Ob46Ih98/"
},
{
"diagram_label": "Stellar spectral types",
"diagram_slug": "Tt35DR10iI63",
"diagram_title": "恒星光譜類型",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "按光譜類型排列的七顆恒星的光譜，從頂部的最熱（O 型）到底部的最冷（M 型）。x 軸錶示光的波長，y 軸錶示該波長接收到的光通量。每個光譜都經過歸一化處理（每個波長的光通量除以該光譜的最大光通量），然後將光譜沿 y 軸相互偏移，以便於觀察。400 納米到 700 納米之間的綫條顔色大緻與人眼看到的該波長光綫的顔色一緻。在 400 納米以下和 700 納米以上，人眼幾乎看不到光，因此這兩條綫的顔色分彆為藍色和紅色。\r\n\r\n較熱的恒星在光譜的藍端有更多的通量，較冷的恒星在紅端有更多的通量。不過，恒星發射的通量總量取決於它的大小和溫度。因此，一顆熱恒星發齣的紅光會比同樣大小的冷恒星多，即使冷恒星發齣的光幾乎都是紅光，但由於上文提到的歸一化處理，這一點在本圖中並不明顯。光譜中的尖銳窄滴是由恒星大氣中的原子和離子引起的吸收綫。光譜綫的強度取決於恒星大氣的溫度。以波長 656.5 納米的氫綫為例。該圖中的所有恒星都主要由氫構成，但對於最熱和最冷的恒星來說，656.5 nm處的氫綫很弱，而對於光譜類型為A和F的恒星來說，氫綫最強。這是因為在A和F恒星大氣層的溫度下，氫在656.5 nm處比在較熱或較冷的恒星中吸收更多的光。\r\n\r\n這裏最冷的恒星，即 M 型恒星，其光譜中的吸收帶很寬。這是因為這顆恒星足夠冷，大氣中含有氧化鈦等化閤物。這些化閤物在天文學中通常被稱為分子，它們會産生比原子或離子更寬的光譜吸收特徵。",
"alt_text": "七條綫。每條綫的峰值從上一條綫的短波長移動到下一條綫的長波長。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-lines_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-lines_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/Tt35DR10iI63/"
},
{
"diagram_label": "Stellar spectral types",
"diagram_slug": "Tt35DR10iI63",
"diagram_title": "恒星光谱类型",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "按光谱类型排列的七颗恒星的光谱，从顶部的最热（O 型）到底部的最冷（M 型）。x 轴表示光的波长，y 轴表示该波长接收到的光通量。每个光谱都经过归一化处理（每个波长的光通量除以该光谱的最大光通量），然后将光谱沿 y 轴相互偏移，以便于观察。400 纳米到 700 纳米之间的线条颜色大致与人眼看到的该波长光线的颜色一致。在 400 纳米以下和 700 纳米以上，人眼几乎看不到光，因此这两条线的颜色分别为蓝色和红色。\r\n\r\n较热的恒星在光谱的蓝端有更多的通量，较冷的恒星在红端有更多的通量。不过，恒星发射的通量总量取决于它的大小和温度。因此，一颗热恒星发出的红光会比同样大小的冷恒星多，即使冷恒星发出的光几乎都是红光，但由于上文提到的归一化处理，这一点在本图中并不明显。光谱中的尖锐窄滴是由恒星大气中的原子和离子引起的吸收线。光谱线的强度取决于恒星大气的温度。以波长 656.5 纳米的氢线为例。该图中的所有恒星都主要由氢构成，但对于最热和最冷的恒星来说，656.5 nm处的氢线很弱，而对于光谱类型为A和F的恒星来说，氢线最强。这是因为在A和F恒星大气层的温度下，氢在656.5 nm处比在较热或较冷的恒星中吸收更多的光。\r\n\r\n这里最冷的恒星，即 M 型恒星，其光谱中的吸收带很宽。这是因为这颗恒星足够冷，大气中含有氧化钛等化合物。这些化合物在天文学中通常被称为分子，它们会产生比原子或离子更宽的光谱吸收特征。",
"alt_text": "七条线。每条线的峰值从上一条线的短波长移动到下一条线的长波长。",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-lines_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-lines_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/Tt35DR10iI63/"
},
{
"diagram_label": "Stellar spectral types - bands",
"diagram_slug": "W970mQ74LZ29",
"diagram_title": "恒星光譜類型 - 波段",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "按光譜類型排列的七顆恒星的光譜，從頂部的最熱（O 型）到底部的最冷（M 型）。x 軸顯示的是光的波長，而每個波長上的亮度或暗度則與該波長上恒星接收到的光通量相對應，較暗的部分光通量較小，較亮的部分光通量較大。每個光譜都進行瞭歸一化處理（每個波長的光通量除以該光譜的最大光通量），因此所有光譜的最大光通量應該具有相同的亮度。在 400 納米到 700 納米之間繪製的顔色與人眼看到的該波長光的顔色基本一緻。在 400 納米以下和 700 納米以上，人眼幾乎看不到光，因此這兩條綫分彆用藍色和紅色錶示。\r\n\r\n較熱的恒星在光譜的藍端有更多的通量，較冷的恒星在紅端有更多的通量。不過，恒星發射的通量總量取決於它的大小和溫度。因此，一顆熱恒星發齣的紅光會比同樣大小的冷恒星多，即使冷恒星發齣的光幾乎都是紅光，但由於上文提到的歸一化處理，這一點在本圖中並不明顯。光譜中的暗窄斑塊是恒星大氣中的原子和離子造成的吸收綫。光譜綫的強度取決於恒星大氣的溫度。以波長 656.5 納米的氫綫為例。該圖中的所有恒星都主要由氫構成，但對於最熱和最冷的恒星來說，656.5 nm處的氫綫很弱，而對於光譜類型為A和F的恒星來說，氫綫最強。這是因為在A和F恒星大氣層的溫度下，氫在656.5 nm處比在較熱或較冷的恒星中吸收更多的光。\r\n\r\n這裏最冷的恒星，即 M 型恒星，其光譜中的吸收帶很寬。這是因為這顆恒星足夠冷，大氣中含有氧化鈦等化閤物。這些化閤物在天文學中通常被稱為分子，它們會産生比原子或離子更寬的光譜吸收特徵。",
"alt_text": "七個條帶，有亮有暗。最亮的部分從頂部的藍色帶移動到底部的紅色帶",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hant",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-bands_zh-hant.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-bands_zh-hant.pdf",
"diagram_url": "https://astro4edu.org/zh-hant/resources/diagram/W970mQ74LZ29/"
},
{
"diagram_label": "Stellar spectral types - bands",
"diagram_slug": "W970mQ74LZ29",
"diagram_title": "恒星光谱类型 - 波段",
"glossary_terms": [
325,
328,
382
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "按光谱类型排列的七颗恒星的光谱，从顶部的最热（O 型）到底部的最冷（M 型）。x 轴显示的是光的波长，而每个波长上的亮度或暗度则与该波长上恒星接收到的光通量相对应，较暗的部分光通量较小，较亮的部分光通量较大。每个光谱都进行了归一化处理（每个波长的光通量除以该光谱的最大光通量），因此所有光谱的最大光通量应该具有相同的亮度。在 400 纳米到 700 纳米之间绘制的颜色与人眼看到的该波长光的颜色基本一致。在 400 纳米以下和 700 纳米以上，人眼几乎看不到光，因此这两条线分别用蓝色和红色表示。\r\n\r\n较热的恒星在光谱的蓝端有更多的通量，较冷的恒星在红端有更多的通量。不过，恒星发射的通量总量取决于它的大小和温度。因此，一颗热恒星发出的红光会比同样大小的冷恒星多，即使冷恒星发出的光几乎都是红光，但由于上文提到的归一化处理，这一点在本图中并不明显。光谱中的暗窄斑块是恒星大气中的原子和离子造成的吸收线。光谱线的强度取决于恒星大气的温度。以波长 656.5 纳米的氢线为例。该图中的所有恒星都主要由氢构成，但对于最热和最冷的恒星来说，656.5 nm处的氢线很弱，而对于光谱类型为A和F的恒星来说，氢线最强。这是因为在A和F恒星大气层的温度下，氢在656.5 nm处比在较热或较冷的恒星中吸收更多的光。\r\n\r\n这里最冷的恒星，即 M 型恒星，其光谱中的吸收带很宽。这是因为这颗恒星足够冷，大气中含有氧化钛等化合物。这些化合物在天文学中通常被称为分子，它们会产生比原子或离子更宽的光谱吸收特征。",
"alt_text": "七个条带，有亮有暗。最亮的部分从顶部的蓝色带移动到底部的红色带",
"credit_text": "IAU OAE/SDSS/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/stellar_spectra_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "zh-hans",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/spectra-bands_zh-hans.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/spectra-bands_zh-hans.pdf",
"diagram_url": "https://astro4edu.org/zh-hans/resources/diagram/W970mQ74LZ29/"
},
{
"diagram_label": "Blackbody Radiation",
"diagram_slug": "8m97bG23XT57",
"diagram_title": "Radiación de cuerpo negro",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Las curvas de radiación emitida por cuerpos negros de diferentes temperaturas. El eje-x muestra la longitud de onda y el eje-y la cantidad de energía emitida cada segundo por un metro cuadrado de la superficie de ese cuerpo negro a cada longitud de onda.\r\n\r\nCuanto más caliente está el cuerpo, más corta es la longitud de onda y más azul es la luz con la que emite su máxima cantidad de energía. A pesar de que el cuerpo más frío de este gráfico tiene un pico de luz roja, los demás cuerpos más calientes emiten más luz roja que el cuerpo más frío.",
"alt_text": "Tres curvas con la radiación en el eje-y y la longitud de onda en el eje-x. Las curvas más frías tienen picos más rojos y más bajos.",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/8m97bG23XT57/"
},
{
"diagram_label": "Blackbody Radiation - UV Catastrophe",
"diagram_slug": "p90iM23hm85",
"diagram_title": "Radiación de cuerpo negro - Catástrofe UV",
"glossary_terms": [
42,
96,
382
],
"categories": [
"Physics"
],
"category_ids": [
16
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Las curvas de radiación emitida por cuerpos negros de diferentes temperaturas. El eje-x muestra la longitud de onda y el eje-y la cantidad de energía emitida cada segundo por un metro cuadrado de la superficie de ese cuerpo negro a cada longitud de onda.\r\n\r\nCuanto más caliente está el cuerpo, más corta es la longitud de onda y más azul es la luz con la que emite su máxima cantidad de energía. A pesar de que el cuerpo más frío de este gráfico tiene un pico de luz roja, los demás cuerpos más calientes emiten más luz roja que el cuerpo más frío.\r\n\r\nLa línea punteada muestra la radiación emitida predicha por la teoría clásica anterior a la mecánica cuántica moderna. Esta predicción tiende a infinito en las longitudes de onda más cortas para cualquier temperatura del cuerpo negro superior a cero y se denominó \"catástrofe ultravioleta\".",
"alt_text": "Tres curvas con la radiación en el eje-y y la longitud de onda en el eje-x. Las curvas más frías tienen picos más rojos y más bajos.",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/blackbody_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/blackbody-radiation-ultraviolet-catastrophe_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/blackbody-radiation-ultraviolet-catastrophe_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/p90iM23hm85/"
},
{
"diagram_label": "Andromeda Constellation Map",
"diagram_slug": "6P43LB422a75",
"diagram_title": "Andromeda Constellation Map",
"glossary_terms": [
7,
8,
15,
66,
78,
256,
286,
466
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Andromeda showing the bright stars and surrounding constellations. Andromeda is surrounded by (going clockwise from the top) Cassiopeia, Lacerta, Pegasus, Pisces, Aries, Triangulum and Perseus. The brightest star in Andromeda (Alpheratz) is in the lower part of the constellation. Together with three stars in Pegasus it forms the asterism known as the \"Great Square of Pegasus\". The next two bright stars in the constellation (Mirach and Almach) form a line extending north-east from Alpheratz.\r\n\r\nAndromeda is a northern constellation and is most visible in the evenings in the Northern Hemisphere autumn. It is visible from all of the Northern Hemisphere and most temperate regions of the Southern Hemisphere but is not visible from Antarctic and Subantarctic regions.\r\n\r\nThe most famous object in Andromeda, the Andromeda Galaxy is marked here with a red ellipse and its Messier catalog number M31.\r\n\r\nThe yellow circle on the left marks the position of the open cluster NGC 752 and the green circle on the right marks NGC 7662 (the blue snowball nebula), a planetary nebula.\r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the lines joining the stars appear on the sky.",
"alt_text": "The bright stars in Andromeda form a Y-shape. Pegasus to the lower right. In the center is M31, marked with a red ellipse.",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/andromeda-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/andromeda-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/6P43LB422a75/"
},
{
"diagram_label": "Andromeda Constellation Map",
"diagram_slug": "6P43LB422a75",
"diagram_title": "Mapa da Constelação de Andrômeda",
"glossary_terms": [
7,
8,
15,
66,
78,
256,
286,
466
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "A constelação de Andrômeda mostrando as estrelas brilhantes e as constelações vizinhas. Andrômeda é cercada por (no sentido horário a partir do topo) Cassiopeia, Lacerta, Pegasus, Peixes, Áries, Triângulo e Perseu. A estrela mais brilhante de Andrômeda (Alpheratz) está na parte inferior da constelação. Juntamente com três estrelas em Pegasus, ela forma o asterismo conhecido como o \"Grande Quadrado de Pegasus\". As próximas duas estrelas brilhantes da constelação (Mirach e Almach) formam uma linha que se estende a nordeste de Alpheratz.\r\n\r\nAndrômeda é uma constelação do norte e é mais visível nas noites de outono do Hemisfério Norte. É visível de todo o hemisfério norte e da maioria das regiões temperadas do hemisfério sul, mas não é visível das regiões antárticas e subantárticas.\r\n\r\nO objeto mais famoso de Andrômeda, a Galáxia de Andrômeda, está marcado aqui com uma elipse vermelha e seu número de catálogo Messier M31.\r\n\r\nO círculo amarelo à esquerda marca a posição do aglomerado aberto NGC 752 e o círculo verde à direita marca a NGC 7662 (a nebulosa bola de neve azul), uma nebulosa planetária.\r\n\r\nO eixo y desse diagrama está em graus de declinação, com o norte para cima, e o eixo x está em horas de ascensão reta, com o leste à esquerda. Os tamanhos das estrelas marcadas aqui estão relacionados à magnitude aparente da estrela, uma medida de seu brilho aparente. Os pontos maiores representam estrelas mais brilhantes. As letras gregas marcam as estrelas mais brilhantes da constelação. Elas são classificadas por brilho, com a estrela mais brilhante sendo rotulada como alfa, a segunda mais brilhante como beta etc., embora essa ordem nem sempre seja seguida exatamente.",
"alt_text": "As estrelas brilhantes em Andrômeda formam um Y. Pegasus no canto inferior direito. No centro está M31, marcado com uma elipse vermelha.",
"credit_text": "Adaptado pelo Escritório de Astronomia para Educação da IAU a partir do original da IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "pt-br",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/andromeda-constellation-map_pt-br.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/andromeda-constellation-map_pt-br.pdf",
"diagram_url": "https://astro4edu.org/pt-br/resources/diagram/6P43LB422a75/"
},
{
"diagram_label": "Andromeda Constellation Map",
"diagram_slug": "6P43LB422a75",
"diagram_title": "Mappa della costellazione di Andromeda",
"glossary_terms": [
7,
8,
15,
66,
78,
256,
286,
466
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "La costellazione di Andromeda mostra le stelle luminose e le costellazioni circostanti. Andromeda è circondata da (in senso orario dall'alto) Cassiopea, Lacerta, Pegaso, Pesci, Ariete, Triangolo e Perseo. La stella più luminosa di Andromeda (Alpheratz) si trova nella parte inferiore della costellazione. Insieme a tre stelle di Pegaso forma l'asterismo noto come \"Grande Quadrato di Pegaso\". Le due successive stelle luminose della costellazione (Mirach e Almach) formano una linea che si estende a nord-est da Alpheratz.\r\n\r\nAndromeda è una costellazione settentrionale ed è maggiormente visibile nelle ore serali dell'autunno dell'emisfero settentrionale. È visibile da tutto l'emisfero settentrionale e dalla maggior parte delle regioni temperate dell'emisfero meridionale, ma non è visibile dalle regioni antartiche e subantartiche.\r\n\r\nL'oggetto più famoso di Andromeda, la Galassia di Andromeda, è contrassegnato da un'ellisse rossa e dal numero di catalogo Messier M31.\r\n\r\nIl cerchio giallo a sinistra indica la posizione dell'ammasso aperto NGC 752 e il cerchio verde a destra indica NGC 7662 (la nebulosa blu a palla di neve), una nebulosa planetaria.\r\n\r\nL'asse y di questo diagramma è in gradi di declinazione, con il nord in alto, mentre l'asse x è in ore di ascensione retta, con l'est a sinistra. Le dimensioni delle stelle qui segnate si riferiscono alla magnitudine apparente della stella, una misura della sua luminosità apparente. I punti più grandi rappresentano le stelle più luminose. Le lettere greche indicano le stelle più luminose della costellazione. Queste sono classificate in base alla luminosità: la stella più luminosa è etichettata come alfa, la seconda più luminosa come beta e così via, anche se questo ordine non viene sempre seguito esattamente.",
"alt_text": "Le stelle luminose di Andromeda compongono una forma a Y. Pegasus in basso a destra. Al centro si trova M31, contrassegnata da un'ellisse rossa.",
"credit_text": "Adattato dall'Ufficio IAU dell'astronomia per l'educazione dall'originale di IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "it",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/andromeda-constellation-map_it.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/andromeda-constellation-map_it.pdf",
"diagram_url": "https://astro4edu.org/it/resources/diagram/6P43LB422a75/"
},
{
"diagram_label": "Andromeda Constellation Map",
"diagram_slug": "6P43LB422a75",
"diagram_title": "Mapa de la constelación de Andrómeda",
"glossary_terms": [
7,
8,
15,
66,
78,
256,
286,
466
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "La constelación de Andrómeda muestra las estrellas brillantes y las constelaciones circundantes. Andrómeda está rodeada por (en el sentido de las agujas del reloj desde arriba) Casiopea, Lacerta, Pegaso, Piscis, Aries, Triángulo y Perseo. La estrella más brillante de Andrómeda (Alpheratz) se encuentra en la parte inferior de la constelación. Junto con tres estrellas de Pegaso forma el asterismo conocido como el \"Gran Cuadrado de Pegaso\". Las dos siguientes estrellas brillantes de la constelación (Mirach y Almach) forman una línea que se extiende hacia el noreste desde Alpheratz.\r\n\r\nAndrómeda es una constelación boreal y es más visible por las tardes en el otoño del hemisferio norte. Es visible desde todo el hemisferio norte y desde la mayoría de las regiones templadas del hemisferio sur, pero no desde las regiones antárticas y subantárticas.\r\n\r\nEl objeto más famoso de Andrómeda, la Galaxia de Andrómeda, está marcado aquí con una elipse roja y su número de catálogo Messier M31.\r\n\r\nEl círculo amarillo de la izquierda marca la posición del cúmulo abierto NGC 752 y el círculo verde de la derecha marca NGC 7662 (la nebulosa azul de la bola de nieve), una nebulosa planetaria.\r\n\r\nEl eje-y de este diagrama está en grados de declinación y con el norte hacia arriba y el eje-x está en horas de ascensión recta con el este a la izquierda. El tamaño de las estrellas marcadas aquí está relacionado con su magnitud aparente, una medida de su brillo aparente. Los puntos más grandes representan estrellas más brillantes. Las letras griegas indican las estrellas más brillantes de la constelación. Están ordenadas por brillo: la estrella más brillante es la alfa, la segunda más brillante es la beta, etc., aunque este orden no siempre se sigue con exactitud.",
"alt_text": "Las estrellas brillantes de Andrómeda forman una Y. Pegaso abajo a la derecha. En el centro está M31, marcada con una elipse roja.",
"credit_text": "Adaptado por la Oficina de Astronomía para la Educación de la UAI a partir del original de IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "es",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/andromeda-constellation-map_es.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/andromeda-constellation-map_es.pdf",
"diagram_url": "https://astro4edu.org/es/resources/diagram/6P43LB422a75/"
},
{
"diagram_label": "Andromeda Constellation Map",
"diagram_slug": "6P43LB422a75",
"diagram_title": "خريطة كوكبة أندروميدا",
"glossary_terms": [
7,
8,
15,
66,
78,
256,
286,
466
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "كوكبة المرأة المسلسلة (او أندروميدا ) تُظهِر النجوم اللامعة والكوكبات المحيطة بها. تحيط بها (باتجاه عقارب الساعة من الأعلى) كوكبة ذات الكرسي، السحلية، الفرس الأعظم، الحوت، الحمل، المثلت، حامل رأس الغول. ألمع نجم في المرأة المسلسلة يقع في الجزء السفلي من الكوكبة. مع ثلاثة نجوم في الفرس الأعظم، يشكل إلفا الفرس المرأة المسلسلة التشكيل النجمي المعروف باسم \"المربع الكبير للفرس الاعظم\". النجمان اللامعان التاليان في الكوكبة (بطن الحوت ونجم الماعز) يشكلان خطاً يمتد شمال شرق من إلفا الفرس المرأة المسلسلة. \r\nأندروميدا هي كوكبة شمالية وتكون مرئية بشكل أفضل في أمسيات الخريف في نصف الكرة الشمالي. يمكن رؤيتها من جميع أنحاء نصف الكرة الشمالي ومعظم المناطق المعتدلة في نصف الكرة الجنوبي، لكنها غير مرئية من المناطق القطبية الجنوبية وما تحت القطب الجنوبي.\r\nأشهر جسم في أندروميدا هو مجرة أندروميدا، المعلَّمة هنا بإلشكل البيضوي الاحمر ورقم الكتالوج مسييه M31. الدائرة الصفراء على اليسار تُظهِر موضع التجمع المفتوح NGC 752 والدائرة الخضراء على اليمين تُظهِر NGC 7662 (سديم كرة الثلج الأزرق)، وهو سديم كوكبي. المحور الرأسي لهذا الرسم البياني بالدرجات من الميل السماوي مع الشمال في الأعلى، والمحور الأفقي بالساعات من المطلع المستقيم مع الشرق إلى اليسار. أحجام النجوم المعلمة هنا تتعلق بالقدر الظاهري للنجوم، وهو مقياس لسطوعها الظاهري. تمثل النقاط الأكبر النجوم الأشد سطوعاً. الحروف اليونانية تشير إلى ألمع النجوم في الكوكبة. هذه النجوم مرتبة حسب السطوع، حيث يُعَلم ألمع نجم بالحرف ألفا، وثاني ألمع نجم بالحرف بيتا، وهكذا، على الرغم من أن هذا الترتيب لا يُتبع دائمًا بشكل دقيق.",
"alt_text": "النجوم اللامعة في كوكبة أندروميدا تشكل حرف Y. كوكبة الفرس الأعظم تقع إلى أسفل اليمين. في المركز توجد مجرة (M31)، المعلَّمة بالشكل البيضوي الاحمر",
"credit_text": "تم تعديله من قِبل مكتب اتحاد الفلك الدولي لتعليم الفلك، استناداً إلى النسخة الأصلية المقدمة من اتحاد الفلك الدولي ومجلة سكاي آند تلسكوب",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "ar",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/andromeda-constellation-map_ar.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/andromeda-constellation-map_ar.pdf",
"diagram_url": "https://astro4edu.org/ar/resources/diagram/6P43LB422a75/"
},
{
"diagram_label": "Hertzsprung-Russell diagram",
"diagram_slug": "iq40Hc92ni31",
"diagram_title": "Hertzsprung-Russell diagram",
"glossary_terms": [
46,
59,
130,
143,
180,
186,
334,
347,
386,
440,
481,
503
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "This diagram shows the temperature and luminosity of different stars. The size of each point represents the star’s radius and its colour is the colour the human eye would see. The stars range in colour from a washed-out blue to a washed-out reddish-orange. No star has a pure colour like red, green or blue as stars’ spectra include light from lots of different colours. However the reddest stars are commonly referred to as red and the bluest stars as blue. The sample of stars used to make this diagram was chosen to show a wide range of stars of different types so the relative number of each type of star is not representative of how commonly each type is found.\r\n \r\nFrom the top left to bottom right there is a long line of stars burning hydrogen in their cores. This is called the main sequence. On this line, one sees the stars Mintaka, Achenar, Sirius A, the Sun and Proxima Centauri. The objects around Proxima Centauri at the lower right end of the main sequence are known as red dwarfs. To the lower right of the red dwarfs are Teide 1 and Kelu-1 A. These two objects are brown dwarfs, objects too low in mass to have cores hot enough to fuse hydrogen for a sustained period of time. As they do not burn hydrogen, brown dwarfs are not considered main sequence stars. The name brown dwarf is unrelated to their colour.\r\n \r\nAbove the main sequence, we find subgiants, giants and supergiants. These are stars that have finished burning hydrogen in their core and have evolved into larger objects. A star’s brightness depends on its temperature and size so giant stars are brighter than stars with a smaller radius but the same temperature. In time these objects will move towards the end of their lives and undergo either a planetary nebula phase or become supernovae. Stars which end their lives with a planetary nebula phase become a type of stellar remnant called a white dwarf. Such objects are much smaller than stars of the same temperature and thus are fainter and are found significantly below the main sequence. Stars which end their lives as supernovae become either black holes or neutron stars. These are not shown on this plot.",
"alt_text": "A line of stars goes from cool faint stars to hot bright stars. Some stars lie above or below this line",
"credit_text": "IAU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/hr_diagram_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/hr_diagram_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/hr_diagram_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/iq40Hc92ni31/"
},
{
"diagram_label": "Crux Constellation Map",
"diagram_slug": "Hj32Ua273O7",
"diagram_title": "Crux Constellation Map",
"glossary_terms": [
15,
50,
66,
78,
286,
318,
466,
518
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Crux (commonly known as the Southern Cross or Crux Australis) showing its bright stars and surrounding constellations. The Southern Cross is surrounding by (going clockwise from the top) Centaurus, Carina and Musca. The brightest star is alpha Crucis which appears at the bottom of the constellation's famous kite shape. The Southern Cross is visible from southern and equatorial regions of the world. In more southerly parts of the world it is circumpolar so is always above the horizon. In other parts of the southern hemisphere and in equatorial regions it is most visible in the evenings in the southern hemisphere autumn.\r\n\r\nThe yellow circles show the locations of two open clusters, NGC 4755 (known as the Jewel Box) and NGC 4609.\r\n\r\nThe line joining gamma and alpha Crucis (the third and first brightest stars in the Southern Cross) points in the approximate direction of the South Celestial Pole. This has led to the Southern Cross playing an important role in celestial navigation, allowing navigators from different astronomical traditions to find their bearings.\r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the lines joining the stars appear on the sky.",
"alt_text": "The four bright stars of Crux form a kite shape with the long axis pointing vertically",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope.",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/crux-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/crux-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/Hj32Ua273O7/"
},
{
"diagram_label": "Andromeda Constellation Map",
"diagram_slug": "6P43LB422a75",
"diagram_title": "Carte de la constellation d'Andromède",
"glossary_terms": [
7,
8,
15,
66,
78,
256,
286,
466
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "La constellation d'Andromède montrant ses étoiles brillantes et les constellations environnantes. Andromède est entourée (dans le sens des aiguilles d'une montre à partir du haut) de Cassiopée, du Lézard, de Pégase, des Poissons, du Bélier, du Triangle et de Persée. L'étoile la plus brillante d'Andromède (Alpheratz) se trouve dans la partie inférieure de la constellation. Avec trois étoiles de Pégase, elle forme l'astérisme connu sous le nom de \"Grand carré de Pégase\". Les deux autres étoiles brillantes de la constellation (Mirach et Almach) forment une ligne qui s'étend au nord-est d'Alpheratz.\r\n\r\nAndromède est une constellation septentrionale et est surtout visible le soir, à l'automne dans l'hémisphère nord. Elle est visible depuis tout l'hémisphère nord et la plupart des régions tempérées de l'hémisphère sud, mais n'est pas visible depuis les régions antarctiques et subantarctiques.\r\n\r\nL'objet le plus célèbre d'Andromède, la galaxie d'Andromède, est marqué ici d'une ellipse rouge et de son numéro de catalogue Messier M31.\r\n\r\nLe cercle jaune à gauche indique la position de l'amas ouvert NGC 752 et le cercle vert à droite indique NGC 7662 (la nébuleuse de la boule de neige bleue), une nébuleuse planétaire.\r\n\r\nL'axe des y de ce diagramme est en degrés de déclinaison avec le nord en haut et l'axe des x est en heures d'ascension droite avec l'est à gauche. La taille des étoiles marquées ici correspond à la magnitude apparente de l'étoile, une mesure de sa luminosité apparente. Les points les plus gros représentent les étoiles les plus brillantes. Les lettres grecques indiquent les étoiles les plus brillantes de la constellation. Elles sont classées par ordre de luminosité, l'étoile la plus brillante étant étiquetée alpha, la deuxième plus brillante bêta, etc., bien que cet ordre ne soit pas toujours respecté à la lettre. Les lignes pointillées marquent les délimitations des constellations selon l'UAI et les lignes vertes pleines marquent l'une des formes couramment utilisées pour représenter les figures des constellations. Ni les limites des constellations, ni les lignes reliant les étoiles n'apparaissent sur le ciel.",
"alt_text": "Les étoiles brillantes d'Andromède forment un Y. Pégase en bas à droite. Au centre se trouve M31, marquée d'une ellipse rouge.",
"credit_text": "Adapté par le Bureau de l'astronomie pour l'éducation de l'AIU à partir de l'original de l'AIU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/andromeda-constellation-map_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/andromeda-constellation-map_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/6P43LB422a75/"
},
{
"diagram_label": "Hertzsprung-Russell diagram",
"diagram_slug": "iq40Hc92ni31",
"diagram_title": "Diagramme de Hertzsprung-Russell",
"glossary_terms": [
46,
59,
130,
143,
180,
186,
334,
347,
386,
440,
481,
503
],
"categories": [
"Stars"
],
"category_ids": [
2
],
"big_ideas": [],
"big_ideas_subidea": [],
"big_ideas_subidea_ids": [],
"caption": "Ce diagramme montre la température et la luminosité de différentes étoiles. La taille de chaque point représente le rayon de l'étoile et sa couleur est celle que l'œil humain verrait. La couleur des étoiles varie d'un bleu délavé à un orange rougeâtre délavé. Aucune étoile n'a une couleur pure comme le rouge, le vert ou le bleu, car les spectres des étoiles contiennent de la lumière de nombreuses couleurs différentes. Toutefois, les étoiles les plus rouges sont communément appelées \"rouges\" et les étoiles les plus bleues \"bleues\". L'échantillon d'étoiles utilisé pour réaliser ce diagramme a été choisi pour présenter un large éventail d'étoiles de différents types. Le nombre relatif de chaque type d'étoile n'est donc pas représentatif de la fréquence de chaque type.\r\n \r\n Du haut à gauche au bas à droite, on observe une longue ligne d'étoiles brûlant de l'hydrogène dans leur cœur. C'est ce qu'on appelle la séquence principale. Sur cette ligne, on trouve les étoiles Mintaka, Achenar, Sirius A, le Soleil et Proxima Centauri. En bas à droite de cette ligne se trouvent Teide 1 et Kelu-1 A. Ces deux objets sont des naines brunes, des objets de masse trop faible pour avoir des noyaux suffisamment chauds pour fusionner l'hydrogène pendant une période de temps prolongée. Le nom de naine brune n'est pas lié à leur couleur.\r\n \r\n Au-dessus de la séquence principale, on trouve les sous-géantes, les géantes, les géantes lumineuses et les supergéantes. Il s'agit d'étoiles qui ont fini de brûler de l'hydrogène dans leur cœur et qui ont évolué pour devenir des objets plus gros. La luminosité d'une étoile dépend de sa température et de sa taille. Ainsi, les étoiles géantes sont plus lumineuses que les étoiles ayant un rayon plus petit mais ont la même température. Avec le temps, ces objets atteindront la fin de leur vie et passeront par une phase de nébuleuse planétaire ou deviendront des supernovae. Les étoiles qui terminent leur vie par une phase de nébuleuse planétaire deviennent un type de vestige stellaire appelé naine blanche. Ces objets sont beaucoup plus petits que les étoiles de même température et sont donc moins lumineux ; on les trouve bien en dessous de la séquence principale. Les étoiles qui terminent leur vie en supernovae deviennent soit des trous noirs, soit des étoiles à neutrons. Elles ne sont pas représentées sur ce graphique.",
"alt_text": "Une ligne d'étoiles va des étoiles faibles et froides aux étoiles chaudes et brillantes. Certaines étoiles se trouvent au-dessus ou en-dessous",
"credit_text": "AIU OAE/Niall Deacon",
"credit_url": null,
"generated_from_github_repository": "astro4edu/hr_diagram_plots",
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "fr",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/hr_diagramme_fr.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/hr_diagramme_fr.pdf",
"diagram_url": "https://astro4edu.org/fr/resources/diagram/iq40Hc92ni31/"
},
{
"diagram_label": "Orion Constellation Map",
"diagram_slug": "dg783o76n014",
"diagram_title": "Orion Constellation Map",
"glossary_terms": [
15,
50,
66,
78,
92,
126,
286,
351,
467,
485
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Orion along with its bright stars and surrounding constellations. Orion is surrounded by (going clockwise from the top) Taurus, Eridanus, Lepus, Monoceros and Gemini. Orion’s brightest stars Betelgeuse and Rigel appear at the northern (upper on this diagram) and southern (lower) end of the constellation respectively with the famous three star “belt” in the middle.\r\n\r\nOrion spans the celestial equator and is thus visible at some time in the year from all of planet Earth. In the most arctic or antarctic regions of the world, some parts of the constellation may not be visible. Orion is most visible in the evenings in the northern hemisphere winter and southern hemisphere summer. The blue line above Orion marks the ecliptic, the path the Sun appears to travel across the sky over the course of a year. The Sun never passes through Orion, but one can occasionally find the other planets of the Solar System and the Moon in Orion.\r\n\r\nJust south of Orion’s belt lie two Messier objects M42 (the Orion nebula) and M43, marked by green squares. These nebulae along with M78 (here the green square to the left of the belt) are part of the huge Orion Molecular Cloud Complex. This covers most of the constellation and includes regions where these molecular clouds are collapsing to form young starts. \r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The circle around Betelgeuse indicates that it is a variable star. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the line marking the ecliptic, nor the lines joining the stars appear on the sky.",
"alt_text": "Orion appears as an hourglass-shaped pattern with two strings of stars extending northeast and northwest",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/orion-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/orion-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/dg783o76n014/"
},
{
"diagram_label": "Libra Constellation Map",
"diagram_slug": "9P17by35Gr8",
"diagram_title": "Libra Constellation Map",
"glossary_terms": [
15,
50,
66,
78,
92,
173,
286,
299,
391,
486
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Libra along with its bright stars and surrounding constellations. Libra is surrounded by (going clockwise from the top) Serpens Caput, Virgo, Hydra, Centaurus, Lupus, Scorpius and Ophiuchus. Libra lies on the ecliptic (shown here as a blue line), this is the path the Sun appears to take across the sky over the course of a year. The Sun is in Libra from late October to late November. The other planets of the Solar System can often be found in Libra.\r\n\r\nLibra lies just south of the celestial equator and is thus visible at some time in all but the most arctic regions. Libra is most visible in the evenings in the northern hemisphere late spring/early summer and southern hemisphere late autumn/early winter. \r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the line marking the ecliptic, nor the lines joining the stars appear on the sky.",
"alt_text": "Libra appears as a triangle pointing north (up) with two lines hanging down. It is bisected by the ecliptic running ESE-WNW",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/libra-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/libra-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/9P17by35Gr8/"
},
{
"diagram_label": "Scorpius Constellation Map",
"diagram_slug": "uM753a62k218",
"diagram_title": "Scorpius Constellation Map",
"glossary_terms": [
15,
50,
66,
78,
92,
132,
173,
286,
299,
391,
466,
474,
485
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Scorpius (often commonly called Scorpio) along with its bright stars and surrounding constellations. Scorpius is surrounded by (going clockwise from the top) Ophiuchus, Serpens Caput, Libra, Lupus, Norma, Ara, Corona Australis and Sagittarius. Scorpius’s brightest star Antares appears in the heart of the constellation with the famous tail of Scoprius in the south-east (lower left). Scorpius lies on the ecliptic (shown here as a blue line), this is the path the Sun appears to take across the sky over the course of a year. The Sun only spends a short amount of time in late November in Scorpius. The other planets of the Solar System can often be found in Scorpius.\r\n\r\nScorpius lies south of the celestial equator. The whole constellation is not visible from the most arctic regions of the world with parts of Scorpius obscured for observers in northern parts of Asia, Europe and North America. Scorpius is most visible in the evenings in the northern hemisphere summer and southern hemisphere winter. \r\n\r\nThe yellow circles mark the positions of the open clusters M6, M7 & NGC 6231 while the yellow circles with plus signs superimposed on them mark the globular clusters M4 and M80. \r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The circle around Antares indicates that it is a variable star. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. The blue line marks the ecliptic, the path the Sun appears to travel across the sky over the course of one year. Neither the constellation boundaries, nor the line marking the ecliptic, nor the lines joining the stars appear on the sky.",
"alt_text": "Scorpius appears as a letter T joined to a letter J. The ecliptic runs ESE to WNW and clips one arm of the T",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/scorpius-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/scorpius-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/uM753a62k218/"
},
{
"diagram_label": "Sagittarius Constellation Map",
"diagram_slug": "Ju53nC20Lt23",
"diagram_title": "Sagittarius Constellation Map",
"glossary_terms": [
15,
48,
50,
66,
78,
92,
132,
199,
211,
286,
292,
299,
348,
391,
429,
466,
474
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Sagittarius along with its bright stars and surrounding constellations. Sagittarius is surrounded by (going clockwise from the top) Aquila, Scutum, Serpens Cauda, Ophiuchus, Scorpius, Corona Australis, Telescopium, Microscopium and Capricornus. The brighter stars in Sagittarius form a distinctive teapot shape. Sagittarius lies on the ecliptic (shown here as a blue line), this is the path the Sun appears to take across the sky over the course of a year. The Sun is in Sagittarius from mid December to mid January. The other planets of the Solar System can often be found in Sagittarius.\r\n\r\nSagittarius lies south of the celestial equator. The famous teapot asterism is visible for all but the most arctic regions of the world but the most southerly parts of the constellation are not visible in northern parts of Asia, Europe and North America. Sagittarius is most visible in the evenings in the northern hemisphere summer and southern hemisphere winter. \r\n\r\nThe supermassive black hole Sagittarius A* which lies at the center of our Milky Way Galaxy is sits on the western (here right-hand) edge of Sagittarius. Due to it covering an area at the center of our Galaxy, Sagittarius is home to many star clusters including open clusters (marked here with yellow circles) and globular clusters (marked here with yellow circles with + signs superimposed on them). Three nebulae are also marked here with green squares. \r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the line marking the ecliptic, nor the lines joining the stars appear on the sky.",
"alt_text": "Sagittarius is shaped like a teapot pouring tea south west. The ecliptic runs WSW to ENE at the top of the constellation",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/sagittarius-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/sagittarius-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/Ju53nC20Lt23/"
},
{
"diagram_label": "Capricornus Constellation Map",
"diagram_slug": "J557Ln95hA62",
"diagram_title": "Capricornus Constellation Map",
"glossary_terms": [
15,
48,
50,
66,
78,
92,
132,
286,
391,
428,
474,
494
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Capricornus (commonly called Capricorn) including its bright stars and surrounding constellations. Capricornus is surrounded by (going clockwise from the top) Aquarius, Aquila, Sagittarius, Microscopium and Piscis Austrinus. Capricornus lies on the ecliptic (shown here as a blue line), this is the path the Sun appears to take across the sky over the course of a year. The Sun is in Capricornus from mid January to mid February. The other planets of the Solar System can often be found in Capricornus.\r\n\r\nCapricornus lies just south of the celestial equator and is visible to all observers south of the Arctic Circle. Capricornus is most visible in the evenings in the northern hemisphere autumn and southern hemisphere spring. \r\n\r\nIn the south east (lower left on this diagram) of the constellation one can find the globular cluster M30 (shown here as a yellow circle with a plus sign superimposed on it).\r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the line marking the ecliptic, nor the lines joining the stars appear on the sky.",
"alt_text": "Capricornus appears as a downward pointing isosceles triangle. The ecliptic runs through the center from WSW to ENE",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/capricornus-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/capricornus-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/J557Ln95hA62/"
},
{
"diagram_label": "Aquarius Constellation Map",
"diagram_slug": "qo31xv8AO72",
"diagram_title": "Aquarius Constellation Map",
"glossary_terms": [
15,
48,
50,
66,
78,
92,
132,
252,
256,
286,
391,
428,
466
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Aquarius along with its bright stars and surrounding constellations. Aquarius is surrounded by (going clockwise from the top) Pegasus, Equuleus, Aquila, Capricornus, Piscis Austrinus, Sculptor, Cetus and Pisces. Aquarius lies on the ecliptic (shown here as a blue line), this is the path the Sun appears to take across the sky over the course of a year. The Sun is in Aquarius from mid February to mid March. The other planets of the Solar System can often be found in Aquarius. \r\n\r\nAquarius spans the celestial equator and is thus visible at some time in the year from all of planet Earth. In the most arctic or antarctic regions of the world, some parts of the constellation may not be visible. Aquarius is most visible in the evenings in the northern hemisphere autumn and southern hemisphere spring. \r\n\r\nThe yellow circles with plus symbols superimposed on them mark the globular clusters M2 and M72. The green circles superimposed on plus symbols mark the planetary nebulae NGC 7293 (the Helix Nebula) and NGC 7002 (the Saturn Nebula). M73 (marked with an x symbol) is a coincident grouping of stars previously erroneously classified as an open cluster. \r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the line marking the ecliptic, nor the lines joining the stars appear on the sky.",
"alt_text": "Aquarius appears as a sprawling series of connected lines. The ecliptic runs through its center from WSW to ENE.",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/aquarius-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/aquarius-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/qo31xv8AO72/"
},
{
"diagram_label": "Pisces Constellation Map",
"diagram_slug": "5t4fz51Q587",
"diagram_title": "Pisces Constellation Map",
"glossary_terms": [
7,
15,
16,
34,
50,
66,
78,
92,
252,
286,
391,
428
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Pisces along with its bright stars and surrounding constellations. Pisces is surrounded by (going clockwise from the top) Andromeda, Pegasus, Aquarius, Cetus, Aries and Triangulum. Pisces lies on the ecliptic (shown here as a blue line), this is the path the Sun appears to take across the sky over the course of a year. The Sun is in Pisces from mid March to mid April. Thus the Sun is in Pisces at the March equinox. At this point the ecliptic crosses the celestial equator. The Sun’s location at the spring equinox is used to set the zero point of the Right Ascension positional coordinate. The other planets of the Solar System can often be found in Pisces.\r\n\r\nPisces spans the celestial equator and is thus visible at some time in the year from all of planet Earth. In the most arctic or antarctic regions of the world, some parts of the constellation may not be visible. Pisces is most visible in the evenings in the northern hemisphere autumn and southern hemisphere spring \r\n\r\nThe grand design spiral galaxy M74 is marked on this diagram with a small red circle. \r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the line marking the ecliptic, nor the lines joining the stars appear on the sky.",
"alt_text": "Pisces appears as a SW-pointing v-shape with loops at the end of each line. The ecliptic runs WSW to ENE through Pisces.",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/pisces-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/pisces-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/5t4fz51Q587/"
},
{
"diagram_label": "Aries Constellation Map",
"diagram_slug": "4V79cV84bK15",
"diagram_title": "Aries Constellation Map",
"glossary_terms": [
15,
16,
50,
66,
78,
92,
252,
286,
351,
391
],
"categories": [
"Naked Eye Astronomy"
],
"category_ids": [
4
],
"big_ideas": [],
"big_ideas_subidea": [
"1.2"
],
"big_ideas_subidea_ids": [
2
],
"caption": "The constellation Aries along with its bright stars and surrounding constellations. Aries is surrounded by (going clockwise from the top) Triangulum, Pisces, Cetus, Taurus and Perseus. Aries lies on the ecliptic (shown here as a blue line), this is the path the Sun appears to take across the sky over the course of a year. The Sun is in Aries from mid April to mid May. The other planets of the Solar System can often be found in Aries.\r\n\r\nAries lies just north of the celestial equator and is thus visible at some time in the year from all of planet Earth except for the most antarctic regions of the world. Aries is most visible in the evenings in the northern hemisphere winter and southern hemisphere summer. \r\n\r\nThe y-axis of this diagram is in degrees of declination with north as up and the x-axis is in hours of right ascension with east to the left. The sizes of the stars marked here relate to the star's apparent magnitude, a measure of its apparent brightness. The larger dots represent brighter stars. The Greek letters mark the brightest stars in the constellation. These are ranked by brightness with the brightest star being labeled alpha, the second brightest beta, etc., although this ordering is not always followed exactly. The dotted boundary lines mark the IAU's boundaries of the constellations and the solid green lines mark one of the common forms used to represent the figures of the constellations. Neither the constellation boundaries, nor the line marking the ecliptic, nor the lines joining the stars appear on the sky.",
"alt_text": "Aries is mostly stars with only a few bright stars in the constellation’s north joined by a curved line. The ecliptic runs WSW to ENE",
"credit_text": "Adapted by the IAU Office of Astronomy for Education from the original by IAU/Sky & Telescope",
"credit_url": "https://www.iau.org/Iau/Iau/Science/What-we-do/The-Constellations.aspx",
"generated_from_github_repository": null,
"license": "CC-BY-4.0",
"license_url": "https://creativecommons.org/licenses/by/4.0/deed.en",
"language_code": "en",
"multimedia_file": "http://www.astro4edu.org/media/diagrams/multimedia/aries-constellation-map_en.png",
"pdf_file": "http://www.astro4edu.org/media/diagrams/pdf/aries-constellation-map_en.pdf",
"diagram_url": "https://astro4edu.org/resources/diagram/4V79cV84bK15/"
}
]
}
