The core-degenerate scenario for the progenitors of Type Ia supernovae
The core-degenerate scenario for the progenitors of Type Ia supernovae
复制标题
Ia 型超新星前身的核心简并情景
DOI：
10.1093/mnras/stw2646
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发表时间：
2016-10
影响因子：
4.8
通讯作者：
Wu C Y
中科院分区：
文献类型：
--
作者：
Wang B;Zhou W H;Zuo Z Y;Li Y B;Luo X;Zhang J J;Liu D D;Wu C Y
Ia型超新星（SNe Ia）的起源仍然不确定。核心简并（CD）方案已被提出作为一种替代方式的生产Ia超新星。在这种情况下，超新星Ia是由一颗碳氧白色矮星（CO WD）与一颗渐近巨星分支伴星的CO核心合并而形成的。然而，Ia型超新星的出生率仍然没有很好地确定。在这项工作中，我们进行了详细的调查CD方案的基础上的二进制人口合成方法。在这种情况下，超新星Ia的延迟时间基本上在9000万年到25000万年之间，这主要是由于观测到的超新星Ia具有短的和中等的延迟时间，尽管这种情况也会产生一些旧的超新星Ia。同时，我们的工作表明，由于对质量转移的更仔细的处理，在这种情况下，超新星Ia的银河系出生率不超过总超新星Ia的20%。虽然本研究中Ia型超新星的出生率低于Ilkov & Soker的研究，但不能排除CD方案是Ia型超新星形成的可行机制。特别是，来自这个场景的星周物质的SNe Ia贡献了总SNe Ia的0.7-10%，这意味着CD场景可以重现像PTF 11 kx那样观测到的SNe Ia的出生率。我们还发现，SNe Ia发生系统性较早的金属丰度值和它们的出生率增加与金属丰度。
The origin of the progenitors of type Ia supernovae (SNe Ia) is still uncertain. The core-degenerate (CD) scenario has been proposed as an alternative way for the production of SNe Ia. In this scenario, SNe Ia are formed at the final stage of common-envelope evolution from a merger of a carbon-oxygen white dwarf (CO WD) with the CO core of an asymptotic giant branch companion. However, the birthrates of SNe Ia from this scenario are still not well determined. In this work, we performed a detailed investigation on the CD scenario based on a binary population synthesis approach. The SN Ia delay times from this scenario are basically in the range of 90Myr-2500Myr, mainly contributing to the observed SNe Ia with short and intermediate delay times although this scenario can also produce some old SNe Ia. Meanwhile, our work indicates that the Galactic birthrates of SNe Ia from this scenario are no more than 20% of total SNe Ia due to more careful treatment of mass transfer. Although the SN Ia birthrates in the present work are lower than those in Ilkov & Soker, the CD scenario cannot be ruled out as a viable mechanism for the formation of SNe Ia. Especially, SNe Ia with circumstellar material from this scenario contribute to 0.7-10% of total SNe Ia, which means that the CD scenario can reproduce the observed birthrates of SNe Ia like PTF 11kx. We also found that SNe Ia happen systemically earlier for a high value of metallicity and their birthrates increase with metallicity.
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影响因子：
6.5
作者：
G. Nelemans;L. Yungelson;S. P. Zwart;F. Verbunt
通讯作者：
G. Nelemans;L. Yungelson;S. P. Zwart;F. Verbunt
DOI：
10.1086/173565
发表时间：
1994
期刊：
The Astrophysical Journal
影响因子：
--
作者：
F. Timmes;S. Woosley;R. Taam
通讯作者：
F. Timmes;S. Woosley;R. Taam
影响因子：
4.8
作者：
G. Briggs;L. Ferrario;C. Tout;D. Wickramasinghe;J. Hurley
通讯作者：
G. Briggs;L. Ferrario;C. Tout;D. Wickramasinghe;J. Hurley
影响因子：
4.8
作者：
N. Soker;E. García–Berro;L. Althaus
通讯作者：
N. Soker;E. García–Berro;L. Althaus
DOI：
10.1046/j.1365-8711.2002.05038.x
发表时间：
2002-01
影响因子：
4.8
作者：
J. Hurley;C. Tout;O. Pols
通讯作者：
J. Hurley;C. Tout;O. Pols