FINAL FATES OF ROTATING WHITE DWARFS AND THEIR COMPANIONS IN THE SINGLE DEGENERATE MODEL OF TYPE Ia SUPERNOVAE
FINAL FATES OF ROTATING WHITE DWARFS AND THEIR COMPANIONS IN THE SINGLE DEGENERATE MODEL OF TYPE Ia SUPERNOVAE
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DOI：
10.1088/2041-8205/756/1/l4
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发表时间：
2012-07
期刊：
影响因子：
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通讯作者：
I. Hachisu;M. Kato;K. Nomoto
中科院分区：
文献类型：
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作者：
I. Hachisu;M. Kato;K. Nomoto
考虑到质量超过钱德拉塞卡质量的吸积白矮星（WDs）的旋转，我们扩展了Ia型超新星（SNe Ia）祖先的新单简并模型，考虑了两种类型的双星系统：具有主序伴星和具有红巨星（RG）伴星的双星系统。我们给出了超新星Ia的质量分布，其质量范围从1.38到2.3 M☉。这些祖先模型被分配给不同类型的Ia型超新星。较低的质量范围（1.38 M☉< MWD > 1.5 M☉），由刚性旋转支持，对应于正常的Ia型超新星。不同的自旋下降时间可能导致亮度的变化。较大的质量范围（MWD > 1.5 M☉），由差速旋转支持，对应于较亮的Ia型超新星，如SN 1991T。在这种情况下，WD质量的变化可能导致亮度的变化。我们还展示了超新星Ia爆炸伴星的演化状态，并对看不见的伴星提出了限制。特别是在WD+RG系统中，大多数RG伴星在SN Ia爆炸前的自旋下降阶段已经演化为氦/碳-氧WDs。在这种情况下，我们预计在爆炸前后不会有任何明显的伴星特征。我们还将我们的新模型与最近对不可见的snia祖星系（如sn2011fe）的严格约束进行了比较。
Taking into account the rotation of mass-accreting white dwarfs (WDs) whose masses exceed the Chandrasekhar mass, we extend our new single degenerate model for the progenitors of Type Ia supernovae (SNe Ia), accounting for two types of binary systems: those with a main-sequence companion and those with a red-giant (RG) companion. We present a mass distribution of WDs exploding as SNe Ia, where the WD mass ranges from 1.38 to 2.3 M☉. These progenitor models are assigned to various types of SNe Ia. A lower mass range of WDs (1.38 M☉ < MWD ≲ 1.5 M☉), which are supported by rigid rotation, corresponds to normal SNe Ia. A variety of spin-down time may lead to a variation of brightness. A higher mass range of WDs (MWD ≳ 1.5 M☉), which are supported by differential rotation, corresponds to brighter SNe Ia such as SN 1991T. In this case, a variety of the WD mass may lead to a variation of brightness. We also show the evolutionary states of the companion stars at SN Ia explosions and pose constraints on the unseen companions. In the WD+RG systems, in particular, most of the RG companions have evolved to helium/carbon–oxygen WDs in the spin-down phase before the SN Ia explosions. In such a case, we do not expect any prominent signature of the companion immediately before and after the explosion. We also compare our new models with the recent stringent constraints on the unseen progenitors of SNe Ia such as SN 2011fe.