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首页> 外文期刊>The Astrophysical journal >A NEW MODEL FOR PROGENITOR SYSTEMS OF TYPE Ia SUPERNOVAE
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A NEW MODEL FOR PROGENITOR SYSTEMS OF TYPE Ia SUPERNOVAE

机译：超新星Ia型祖先系统的新模型

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摘要

We propose a new Model for progenitor systems of Type Ia supernovae. The Model consists of an accreting white dwarf and a lobe-filling, low-mass red giant. When the mass accretion rate exceeds a certain critical rate, there is no static envelope solution on the white dwarf. For this case, we find a new strong wind solution, which replaces the static envelope solution. Even if the mass-losing star has a deep convective envelope, the strong wind stabilizes the mass transfer until the mass ratio, q, between the mass-losing star and the mass-accreting white dwarf reaches 1.15, i.e., q < 1.15. A part of the transferred matter can be accumulated on the white dwarf at a rate that is limited to M_(cr)= 9.0 X 10~(-7) (M_(WD)/solar mass - 0.50) solar mass yr~(-1), and the rest is blown off in the wind. The photospheric temperature is kept around T～1 X 10~5-2 X 10~5 K during the wind phase. After the wind stops, the temperature quickly increases up to ～1 X 10~6 K. The white dwarf steadily burns hydrogen and accretes helium, thereby being able to increase its mass up to 1.38 solar mass and explode as a Type Ia supernova. The expected birth rate of this type of supernovae is consistent with the observed rate of Type Ia supernovae. The hot white dwarf may not be observed during the strong wind phase due to self-absorption by the wind itself. The Strong wind stops when the mass transfer rate decreases below M_(cr). Then it can be observed as a supersoft X-ray source.
机译：我们为Ia型超新星的祖细胞系统提出了一个新模型。该模型由一个积聚的白矮星和一个充满叶，低质量的红色巨人组成。当质量增长速率超过某个临界速率时，白矮星上没有静态包络线解决方案。对于这种情况，我们找到了一种新的强风解决方案，它取代了静态包络线解决方案。即使质量损失恒星具有较深的对流包层，强风也会稳定质量传递，直到质量损失恒星与质量增加的白矮星之间的质量比q达到1.15，即q <1.15。一部分转移物可以以M_（cr）= 9.0 X 10〜（-7）（M_（WD）/太阳质量-0.50）太阳质量yr〜（- 1），其余的随风飘散。在风期，光球温度保持在T〜1 X 10〜5-2 X 10〜5 K左右。风停止后，温度迅速升高到〜1 X 10〜6K。白矮星稳定地燃烧氢并吸收氦气，从而能够将其质量增加到1.38太阳质量并爆炸成Ia型超新星。这种超新星的预期出生率与Ia型超新星的观测率一致。在强风阶段，由于风自身的自我吸收，可能无法观察到炽热的白矮星。当传质速率降低到M_（cr）以下时，强风停止。然后可以将其观察为超软X射线源。

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