HUNTING FOR THE PROGENITOR OF SN 1006: HIGH-RESOLUTION SPECTROSCOPIC SEARCH WITH THE FLAMES INSTRUMENT
HUNTING FOR THE PROGENITOR OF SN 1006: HIGH-RESOLUTION SPECTROSCOPIC SEARCH WITH THE FLAMES INSTRUMENT
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DOI：
10.1088/0004-637x/759/1/7
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发表时间：
2012-07
期刊：
影响因子：
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通讯作者：
W. E. Kerzendorf;B. Schmidt;J. B. Laird;P. Podsiadlowski;M. Bessell
中科院分区：
文献类型：
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作者：
W. E. Kerzendorf;B. Schmidt;J. B. Laird;P. Podsiadlowski;M. Bessell
Ia型超新星在宇宙演化中起着重要的作用，有着广泛的应用。人们普遍认为这些事件是接近钱德拉塞卡质量（1.38 M☉）的碳氧白矮星的热核爆炸。然而，CO白矮星出生时的质量远低于钱德拉塞卡极限，因此需要质量吸积才能成为Ia型超新星。吸积主要有两种情况：第一种是两颗白矮星的合并，第二种是伴星的稳定质量吸积。根据预测，这颗伴星（也被称为供体星）在爆炸中幸存下来，因此应该在Ia型残留物的中心可见。在本文中，我们仔细观察了SN 1006残骸的中心恒星（总共79颗），以寻找根据这种情况预测的幸存的供体恒星。我们在SN 1006中没有发现符合传统吸积模式的恒星。
Type Ia supernovae play a significant role in the evolution of the universe and have a wide range of applications. It is widely believed that these events are the thermonuclear explosions of carbon–oxygen white dwarfs close to the Chandrasekhar mass (1.38 M☉). However, CO white dwarfs are born with masses much below the Chandrasekhar limit and thus require mass accretion to become Type Ia supernovae. There are two main scenarios for accretion: first, the merger of two white dwarfs and, second, a stable mass accretion from a companion star. According to predictions, this companion star (also referred to as donor star) survives the explosion and thus should be visible in the center of Type Ia remnants. In this paper, we scrutinize the central stars (79 in total) of the SN 1006 remnant to search for the surviving donor star as predicted by this scenario. We find no star consistent with the traditional accretion scenario in SN 1006.