TIDALLY ENHANCED STELLAR WIND: A WAY TO MAKE THE SYMBIOTIC CHANNEL TO TYPE Ia SUPERNOVA VIABLE
TIDALLY ENHANCED STELLAR WIND: A WAY TO MAKE THE SYMBIOTIC CHANNEL TO TYPE Ia SUPERNOVA VIABLE
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DOI：
10.1088/2041-8205/735/2/l31
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发表时间：
2011-06
期刊：
影响因子：
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通讯作者：
Xuefei Chen;Zhanwen Han;C. Tout
中科院分区：
文献类型：
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作者：
Xuefei Chen;Zhanwen Han;C. Tout
在Ia型超新星(SNE Ia)单简并情形的共生(或WD+RG)通道中，爆炸发生在恒星形成后的较长时间。如果没有某种机制来提高白矮星的吸积率，来自这个通道的出生率将太低，无法解释所有观测到的SNE Ia。一种潮汐增强的恒星风可以做到这一点，这种风被认为可以解释与双星系统中的巨星演化有关的许多现象。与质量剥离相比，该模型将SneIa前体的空间扩展到更长的轨道周期，从而将共生通道的出生率提高到约0.0069年的−1。两颗共生星，T CRB和RS Oph，被认为是最有可能通过共生通道产生SNE Ia的恒星，它们恰好位于我们模型预测的周期伴生质量空间内。
In the symbiotic (or WD+RG) channel of the single-degenerate scenario for type Ia supernovae (SNe Ia), the explosions occur a relatively long time after star formation. The birthrate from this channel would be too low to account for all observed SNe Ia were it not for some mechanism to enhance the rate of accretion on to the white dwarf. A tidally enhanced stellar wind, of the type which has been postulated to explain many phenomena related to giant star evolution in binary systems, can do this. Compared to mass stripping, this model extends the space of SNe Ia progenitors to longer orbital periods and hence increases the birthrate to about 0.0069 yr−1 for the symbiotic channel. Two symbiotic stars, T CrB and RS Oph, considered to be the most likely progenitors of SNe Ia through the symbiotic channel, are well inside the period–companion mass space predicted by our models.