论文标题
Chandrasekhar-Mass White Dwarfs是根据核断变约束的一小部分IA型超新星的祖细胞
Chandrasekhar-mass white dwarfs are the progenitors of a small fraction of Type Ia supernovae according to nucleosythesis constraints
论文作者
论文摘要
数十年来，IA型超新星（SNE IA）的精确祖细胞系统（sne ia）是几十年来一直是争论的问题。我们的小组在大规模WD爆炸之前的增生和沸腾阶段进行的最新研究表明，热失控的中央密度在$（3.6-6.3）\ times10^9 $ g cm $^{-3} $范围内，用于合理选择WD和Progenitor and Progenitor and Progenitor and Proginoritic and for。在这项工作中，我们计算了对此类WD爆炸的一维模拟，并特别强调了射流的化学成分，在所有情况下，该化学物质的中性同位素非常丰富（$^{54} $ CR）和钛（$^{50} $ ti）。我们表明，为了使这种核合成与太阳系的同位素丰度调和，Chandrasekhar-Mass White Dwarfs最多可以占正常luminosity sne sne ia的最多26％，或者最多可以占所有SNE IA的20％。
The precise progenitor system of type Ia supernovae (SNe Ia), whether it is a white dwarf (WD) close to the Chandrasekhar limit or substantially less massive, has been a matter of debate for decades. Recent research by our group on the accretion and simmering phases preceding the explosion of a massive WD has shown that the central density at thermal runaway lies in the range $(3.6-6.3)\times10^9$ g cm$^{-3}$ for reasonable choices of accretion rate onto the WD and progenitor metallicity. In this work, we have computed one-dimensional simulations of the explosion of such WDs, with special emphasis on the chemical composition of the ejecta, which in all cases is extremely rich in neutronized isotopes of chromium ($^{54}$Cr) and titanium ($^{50}$Ti). We show that, in order to reconcile such a nucleosynthesis with the isotopic abundances of the Solar System, Chandrasekhar-mass white dwarfs can account for at most 26 per cent of normal-luminosity SNe Ia, or at most 20 per cent of all SNe Ia.
