词条光谱

描述: 光穿过水滴，光线将分成紫色、蓝色、绿色到黄色、橙色和红色的基本颜色，这就形成了彩虹。每种颜色对应一个波长范围，彩虹的颜色是按照从紫到红的波长递增顺序排列的。这种按波长分解的光（或更一般的说法，电磁辐射）被称为光谱。

电磁辐射是由被称为“光子”的光粒子混合而成的。光谱相当于按能量对光子进行分类，并记录每个特定能量范围内有多少光子。根据量子力学的基本定律，这等同于按频率对光进行分类——这是描述光谱的另一种方式。

如果能量随波长（或光子能量，或频率）的变化平滑变化，则称为连续光谱。与此相反，光谱中某些波长处的尖锐凹陷或峰值分别称为吸收线和发射线。这些线是由于原子或分子（甚至原子核）内部不同能级之间的跃迁而产生的，它们会吸收或发射特定波长的辐射。例如，在可见光中，恒星会显示出带有吸收线的连续光谱。这些吸收线包含恒星化学成分的信息。对光谱的分析称为光谱学；能够记录光谱的仪器称为光谱仪、分光计或摄谱仪。

相关词条

用其他语言查看该词条

词条和定义状态： 该术语的英文原始定义已通过天文研究人员和教师的审核
该术语及其定义的译文仍待审核

OAE多语言词汇表是由国际天文学联合会（IAU）天文教育办公室（OAE）和国际天文学联合会（IAU）天文推广办公室（OAO）合作的项目。. 术语和定义由 OAE中心, OAE 国家天文教育协调员（NAECs）以及其他志愿者共同选择、撰写和审阅。您可以在找到完整的致谢列表。所有词汇表术语及其定义均根据 Creative Commons CC BY-4.0许可证发布且版权归属于 “IAU OAE”。

如果您发现此词汇术语或定义中的事实或翻译错误，请向发邮件联系.

相关图表

A smooth line declining at longer wavelengths with a few sharp dips.

Spectrum of an O-type star

图注： 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. The 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.
来源： IAU OAE/SDSS/Niall Deacon

License: CC-BY-4.0 知识共享许可协议署名 4.0 国际 (CC BY 4.0) 图标

Spectrum of a B-type star

图注： 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. The 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.
来源： IAU OAE/SDSS/Niall Deacon

License: CC-BY-4.0 知识共享许可协议署名 4.0 国际 (CC BY 4.0) 图标

A smooth line peaking about 420 nm then declining at longer wavelengths with a few fairly broad dips.

Spectrum of an A-type star

图注： 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. The 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.
来源： IAU OAE/SDSS/Niall Deacon

License: CC-BY-4.0 知识共享许可协议署名 4.0 国际 (CC BY 4.0) 图标

A relatively smooth line peaking about 430 nm then declining at longer wavelengths with a few fairly broad dips.

Spectrum of an F-type star

图注： 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. The 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.
来源： IAU OAE/SDSS/Niall Deacon

License: CC-BY-4.0 知识共享许可协议署名 4.0 国际 (CC BY 4.0) 图标

A quite ragged line peaking about 470 nm then declining at longer wavelengths with a few deeper dips.

Spectrum of a G-type star

图注： 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. The 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.
来源： IAU OAE/SDSS/Niall Deacon

License: CC-BY-4.0 知识共享许可协议署名 4.0 国际 (CC BY 4.0) 图标

Browse all diagrams
for this term