Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae
Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae
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DOI：
10.1051/0004-6361/201630099
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发表时间：
2017-08
影响因子：
6.5
通讯作者：
C. Wu;B. Wang;D. Liu;Z. Han
中科院分区：
文献类型：
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作者：
C. Wu;B. Wang;D. Liu;Z. Han
上下文。Ia型超新星（SNe Ia）在宇宙学和星系化学演化研究中起着至关重要的作用。它们被认为是碳氧白矮星（CO WDs）的热核爆炸，当它们的质量达到钱德拉塞卡质量极限时。先前的研究表明，超新星可能是超新星Ia的祖先候选者。然而，氦新星爆发期间的质量保持效率仍然不确定。目标。在本文中，我们旨在研究氦新星爆发的质量保持效率，并探讨是否可以通过氦新星爆发产生超新星Ia。方法。利用恒星演化代码Modules for Experiments in stellar Astrophysics，模拟了一系列初始质量为0.7 ~ 1.35 M⊙、吸积速率不同的多周期he层闪光现象。结果。我们得到了不同初始质量的氦新星爆发的质量保持效率，可用于双星居群合成研究。在我们的模拟中，氦新星爆发可以使黑洞的质量增加到钱德拉塞卡质量极限，并且可以在黑洞中心触发爆炸性的碳燃烧；这表明氦新星爆发可以产生超新星Ia。同时，本研究的质量保持效率低于以往的研究，这导致Ia型超新星通过WD + He星通道的出生率较低。得到了爆炸燃烧时的元素丰度分布，可作为研究Ia型超新星爆炸模型的初始输入参数。
Context. Type Ia supernovae (SNe Ia) play a crucial role in studying cosmology and galactic chemical evolution. They are thought to be thermonuclear explosions of carbon-oxygen white dwarfs (CO WDs) when their masses reach the Chandrasekar mass limit in binaries. Previous studies have suggested that He novae may be progenitor candidates of SNe Ia. However, the mass retention efficiencies during He nova outbursts are still uncertain. Aims. In this article, we aim to study the mass retention efficiencies of He nova outbursts and to investigate whether SNe Ia can be produced through He nova outbursts. Methods. Using the stellar evolution code Modules for Experiments in Stellar Astrophysics, we simulated a series of multicycle He-layer flashes, in which the initial WD masses range from 0.7 to 1.35 M ⊙ with various accretion rates. Results. We obtained the mass retention efficiencies of He nova outbursts for various initial WD masses, which can be used in the binary population synthesis studies. In our simulations, He nova outbursts can increase the mass of the WD to the Chandrasekar mass limit and the explosive carbon burning can be triggered in the center of the WD; this suggests that He nova outbursts can produce SNe Ia. Meanwhile, the mass retention efficiencies in the present work are lower than those of previous studies, which leads to a lower birthrates of SNe Ia through the WD + He star channel. Furthermore, we obtained the elemental abundances distribution at the moment of explosive carbon burning, which can be used as the initial input parameters in studying explosion models of SNe Ia.