II型超新星的原子核结构与核塌缩的命运
Nuclear Structure and the Fate of Core Collapse (Type II) Supernova
摘要：
很长一段时间里，格里·布朗和他的合作者汉斯·贝特（Hans Bethe）一直在考虑核心坍缩（II型）超新星的最终命运问题。回顾了关于K介子凝聚态的原子核结构和致密核物质的软状态方程的想法，他们得出结论，质量低至17- 18 M $_\odot$（包括超新星1987 A）的祖星可能坍缩成质量略高于1.5 M $_\odot$的小质量黑洞，这是他们推导出的中子星的上限。我们讨论了另一种原子核结构效应，它决定了氦燃烧结束时的碳氧比（C/O）。这个比例也决定了II型超新星的命运，富碳的祖星产生中子星，富氧的坍缩成黑洞。虽然C/O比是恒星演化中最重要的核输入之一，但它仍然没有足够的精确度。我们讨论了未来的努力，测量与γ束和TPC探测器的12 C（a，g）16 O反应，决定恒星氦燃烧的C/O比。
英文摘要：
For a long time Gerry Brown and his collaborator Hans Bethe considered the question of the final fate of a core collapse (Type II) supernova. Recalling ideas from nuclear structure on Kaon condensate and a soft equation of state of the dense nuclear matter they concluded that progenitor stars with mass as low a 17-18M$_\odot$ (including supernova 1987A) could collapse to a small mass black hole with a mass just beyond 1.5M$_\odot$, the upper bound they derive for a neutron star. We discuss another nuclear structure effect that determines the carbon to oxygen ratio (C/O) at the end of helium burning. This ratio also determines the fate of a Type II supernova with a carbon rich progenitor star producing a neutron star and oxygen rich collapsing to a black hole. While the C/O ratio is one of the most important nuclear input to stellar evolution it is still not known with sufficient accuracy. We discuss future efforts to measure with gamma-beam and TPC detector the 12C(a,g)16O reaction that determines the C/O ratio in stellar helium burning.
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