At the core of a planetary nebula, Henize 2-428, two white dwarf stars slightly under one solar mass each are expected to merge and create a Type Ia supernova destroying both in about 700 million years (artist's impression).
A Type Ia supernova (read: "type one-A") is a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf. The other star can be anything from a giant star to an even smaller white dwarf.[1]
Physically, carbon–oxygen white dwarfs with a low rate of rotation are limited to below 1.44 solar masses (M☉).[2][3] Beyond this "critical mass", they reignite and in some cases trigger a supernova explosion; this critical mass is often referred to as the Chandrasekhar mass, but is marginally different from the absolute Chandrasekhar limit, where electron degeneracy pressure is unable to prevent catastrophic collapse. If a white dwarf gradually accretes mass from a binary companion, or merges with a second white dwarf, the general hypothesis is that a white dwarf's core will reach the ignition temperature for carbon fusion as it approaches the Chandrasekhar mass. Within a few seconds of initiation of nuclear fusion, a substantial fraction of the matter in the white dwarf undergoes a runaway reaction, releasing enough energy (1×1044 J)[4] to unbind the star in a supernova explosion.[5]
The Type Ia category of supernova produces a fairly consistent peak luminosity because of the fixed critical mass at which a white dwarf will explode. Their consistent peak luminosity allows these explosions to be used as standard candles to measure the distance to their host galaxies: the visual magnitude of a type Ia supernova, as observed from Earth, indicates its distance from Earth.
^HubbleSite - Dark Energy - Type Ia Supernovae
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Yoon, S.-C.; Langer, L. (2004). "Presupernova Evolution of Accreting White Dwarfs with Rotation". Astronomy and Astrophysics. 419 (2): 623–644. arXiv:astro-ph/0402287. Bibcode:2004A&A...419..623Y. doi:10.1051/0004-6361:20035822. S2CID 2963085. Archived from the original on 2007-10-25. Retrieved 2007-05-30.
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Mazzali, P. A.; Röpke, F. K.; Benetti, S.; Hillebrandt, W. (2007). "A Common Explosion Mechanism for Type Ia Supernovae". Science. 315 (5813): 825–828. arXiv:astro-ph/0702351. Bibcode:2007Sci...315..825M. doi:10.1126/science.1136259. PMID 17289993. S2CID 16408991.
^Li, Miao; Li, Yuan; Bryan, Greg L.; Ostriker, Eve C.; Quataert, Eliot (2020-05-05). "The Impact of Type Ia Supernovae in Quiescent Galaxies. I. Formation of the Multiphase Interstellar Medium". The Astrophysical Journal. 894 (1): 44. arXiv:1909.03138. Bibcode:2020ApJ...894...44L. doi:10.3847/1538-4357/ab86b4. ISSN 0004-637X.
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"Introduction to Supernova Remnants". NASA Goddard/SAO. 2006-09-07. Retrieved 2007-05-01.
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its atmosphere. In this case, the event is usually classified as a TypeIasupernova. Novae most often occur in the sky along the path of the Milky Way...
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and immediately classified as a Type II supernova. TypeIasupernova SN 2011fe from August 2011 Type II supernova SN 2023ixf from May 2023 List of Messier...
visible, and near-infrared to measure the expansion of the universe using TypeIa supernovae, baryon acoustic oscillations, the number of galaxy clusters...
Distant TypeIaSupernova Confirmed By Supernova Analysis At NERSC". Lawrence Berkeley National Laboratory. Adam Riess (2 April 2001). "Farthest Supernova Ever...
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