
TL;DR
Type Ia supernovae are thermonuclear explosions of white dwarfs in binary systems, crucial for cosmology and galactic chemical evolution, but their exact progenitors and explosion mechanisms are still not fully understood.
Contribution
This paper reviews the current understanding of Type Ia supernovae, highlighting uncertainties and the need for further research into their progenitors and explosion mechanisms.
Findings
Confirmed the role of radioactive decay of $^{56}$Ni in luminosity
Evidence suggests multiple progenitor channels
Uncertainties remain about binary companion nature
Abstract
Type Ia supernovae (SNe Ia) correspond to the thermonuclear explosion of a carbon-oxygen white dwarf (C-O WD) star in a binary system, triggered by the accretion of material from another star, or the merger/collision with a secondary WD. Their phenomenal luminosity -- several billion times that of the sun -- has motivated their use as cosmological distance indicators and led to the discovery of the accelerated expansion of the universe. SNe Ia are also the main producers of iron and hence play a fundamental role in the chemical evolution of galaxies. While recent observations have confirmed the basic theoretical picture of an exploding C-O WD star whose luminosity is powered by the radioactive decay of Ni, a number of uncertainties remain concerning the nature of the binary companion and the explosion mechanism. Several lines of evidence point towards the existence of multiple…
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Taxonomy
TopicsGamma-ray bursts and supernovae · Astro and Planetary Science
