This page describes an image The Classical Nova GK Persei
Scarica File ( immagine 5.84 MB)
Didascalia:
This composite image shows the aftermath of a stellar explosion known as a nova, specifically the remnant of a classical nova called GK Persei. A nova occurs when a very dense star called a white dwarf pulls hydrogen-rich gas from a companion star in a binary system until the accumulated material ignites in a powerful thermonuclear explosion. This sudden release of energy sweeps material outward and produces bright X-ray, optical, and radio emission that can be studied long after the blast.
GK Persei was for a very short time in 1901 one of the brightest stars in the sky. Classical novae like GK Persei temporarily brighten dramatically — sometimes to thousands of times their usual luminosity — before fading over months or years as the expanding shell moves through space. In this image taken over 100 years since the nova's 1901 brightening, X-rays (shown in blue) reveal very hot gas left behind by the explosion, optical data (yellow) show clumps of matter ejected from the star’s surface, and radio information (pink) highlights high-energy electrons energized by the expanding nova shock wave. Studying novae helps scientists learn about how stars interact in binary systems and how powerful bursts of energy shape the material around them.
The nature of the pink blob in the lower left is not known.
Didascalie in altre lingue
Crediti per l'immagine: X-ray: NASA/CXC/RIKEN/D.Takei et al; Optical: NASA/STScI; Radio: NRAO/VLA Link per i Crediti
Termini di glossario connessi:
Nova
Licenza per l'immagine: Dominio Pubblico Dominio Pubblico icone
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Didascalie in lingue diverse:
Didascalia: Dieses zusammengesetzte Bild zeigt die Folgen einer als Nova bezeichneten Sternexplosion, genauer gesagt den Überrest einer klassischen Nova namens GK Persei. Eine Nova entsteht, wenn ein sehr dichter Stern, ein sogenannter Weißer Zwerg, wasserstoffreiches Gas von einem Begleitstern in einem Doppelsternsystem ansaugt, bis sich das angesammelte Material in einer gewaltigen thermonuklearen Explosion entzündet. Diese plötzliche Freisetzung von Energie schleudert Material nach außen und erzeugt helle Röntgen-, optische und Radioemissionen, die noch lange nach der Explosion untersucht werden können.
GK Persei war 1901 für eine sehr kurze Zeit einer der hellsten Sterne am Himmel. Klassische Novae wie GK Persei hellen sich vorübergehend dramatisch auf – manchmal auf das Tausendfache ihrer üblichen Leuchtkraft –, bevor sie über Monate oder Jahre hinweg wieder verblassen, während sich die expandierende Hülle durch den Weltraum bewegt. Auf diesem Bild, das über 100 Jahre nach dem Aufhellen der Nova im Jahr 1901 aufgenommen wurde, zeigen Röntgenstrahlen (blau dargestellt) sehr heißes Gas, das von der Explosion zurückgelassen wurde, optische Daten (gelb) zeigen Materieklumpen, die von der Sternoberfläche ausgestoßen wurden, und Radiodaten (rosa) heben hochenergetische Elektronen hervor, die durch die sich ausbreitende Nova-Schockwelle angeregt wurden. Die Erforschung von Novae hilft Wissenschaftlern zu verstehen, wie Sterne in Doppelsternsystemen interagieren und wie gewaltige Energiestöße die Materie um sie herum formen.
Die Natur des rosa Flecks unten links ist unbekannt.
Crediti per l'immagine: Röntgen: NASA/CXC/RIKEN/D. Takei et al.; Optisch: NASA/STScI; Radio: NRAO/VLA
Termini di glossario connessi: Nova Stato di traduzione della didascalia: Non ancora approvato da un revisore
Traduttori della didascalia: Simon Kraus
Didascalia: This composite image shows the aftermath of a stellar explosion known as a nova, specifically the remnant of a classical nova called GK Persei. A nova occurs when a very dense star called a white dwarf pulls hydrogen-rich gas from a companion star in a binary system until the accumulated material ignites in a powerful thermonuclear explosion. This sudden release of energy sweeps material outward and produces bright X-ray, optical, and radio emission that can be studied long after the blast.
GK Persei was for a very short time in 1901 one of the brightest stars in the sky. Classical novae like GK Persei temporarily brighten dramatically — sometimes to thousands of times their usual luminosity — before fading over months or years as the expanding shell moves through space. In this image taken over 100 years since the nova's 1901 brightening, X-rays (shown in blue) reveal very hot gas left behind by the explosion, optical data (yellow) show clumps of matter ejected from the star’s surface, and radio information (pink) highlights high-energy electrons energized by the expanding nova shock wave. Studying novae helps scientists learn about how stars interact in binary systems and how powerful bursts of energy shape the material around them.
The nature of the pink blob in the lower left is not known.
Crediti per l'immagine: X-ray: NASA/CXC/RIKEN/D.Takei et al; Optical: NASA/STScI; Radio: NRAO/VLA
Termini di glossario connessi: Nova
