A progenitor for the extremely luminous Type Ic supernova 2007bi
A progenitor for the extremely luminous Type Ic supernova 2007bi
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DOI：
10.1111/j.1745-3933.2011.01008.x
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发表时间：
2011-01
影响因子：
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通讯作者：
T. Yoshida;H. Umeda
中科院分区：
文献类型：
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作者：
T. Yoshida;H. Umeda
SN2007bi是一颗极其明亮的IC型超新星。这颗超新星被认为是从一颗非常大质量的恒星演化而来的，对于爆炸机制，人们提出了两种可能性。一种可能性是具有MCO∼100MCO核心前驱的对不稳定超新星。另一种可能性是Mco∼为40M�的核心塌缩超新星。我们研究了主序列质量为Mms=100-500M�，Z0=0.004的超大质量恒星的演化，以限制SN2007bi的前身。文中还讨论了与地表氦丰度有关的超新星类型。作为一对不稳定超新星爆发的前驱物质的主序质量可能是∼515-575M�。当考虑质量损失率的不确定性时，最小主序质量可能为310毫秒。一颗MMS110-280M的恒星演化为一颗CO星，适合于SN2007bi的核心塌缩超新星。基于对不稳定性和核心塌缩超新星概率的论证支持SN2007bi起源于核心塌缩超新星事件的假设。
SN 2007bi is an extremely luminous Type Ic supernova. This supernova is thought to be evolved from a very massive star, and two possibilities have been proposed for the explosion mechanism. One possibility is a pair-instability supernova with an MCO ∼ 100 MCO core progenitor. Another possibility is a core-collapse supernova with MCO ∼ 40 M� .W e investigate the evolution of very massive stars with main-sequence mass MMS = 100-500 M� and Z0 = 0.004, which is in the metallicity range of the host galaxy of SN 2007bi, to constrain the progenitor of SN 2007bi. The supernova type relating to the surface He abundance is also discussed. The main-sequence mass of the progenitor exploding as a pair-instability supernova could be MMS ∼ 515-575 M� . The minimum main-sequence mass could be 310 Mwhen uncertainties in the mass-loss rate are considered. A star with MMS ∼ 110-280 Mevolves to a CO star, appropriate for the core-collapse supernova of SN 2007bi. Arguments based on the probability of pair-instability and core-collapse supernovae favour the hypothesis that SN 2007bi originated from a core-collapse supernova event.