arXiv 2008.022962020-08-05astro-ph.HEnucl-th

遥远未来的黑矮星超新星

Black Dwarf Supernova in the Far Future

M. E. Caplan

备注：: 6 pages, 1 figure, accepted for publication in MNRAS
DOI：: 10.1093/mnras/staa2262

摘要：

在遥远的未来，在恒星形成停止后的很长一段时间里，宇宙中将充满稀疏的简并残余物，其中大多数是白矮星，尽管它们的最终命运是一个悬而未决的问题。这些白矮星将冷却并冻结成固态的黑矮星，而致密核聚变将慢慢地将它们的成分加工成铁-56。然而，由于电子分数的下降，这些恒星的拉塞卡极限将降低，最终将低于最大质量的黑矮星。因此，质量大于$\sim 1.2 M_\odot$的孤立矮星将在遥远的未来由于铁-56在其核心的缓慢积累而坍缩。如果质子衰变不发生，那么这就是大约$10^{21}$恒星的最终命运，大约占可观测宇宙中所有恒星的百分之一。我们目前的计算的内部结构的黑矮星与铁的核心作为一个模型的祖先。从致密核融合率，我们估计它们的寿命，因此延迟时间为$10^{1100}$年。我们推测，高质量的黑矮星超新星类似于O/Ne/Mg白矮星的吸积引起的坍缩，而随后的低质量瞬变类似于剥离包层的核心坍缩超新星，可能是热寂之前最后一个有趣的天体物理瞬变。

英文摘要：

In the far future long after star formation has ceased the universe will be populated by sparse degenerate remnants, mostly white dwarfs, though their ultimate fate is an open question. These white dwarfs will cool and freeze solid into black dwarfs while pycnonuclear fusion will slowly process their composition to iron-56. However, due to the declining electron fraction the Chandrasekhar limit of these stars will be decreasing and will eventually be below that of the most massive black dwarfs. As such, isolated dwarf stars with masses greater than $\sim 1.2 M_\odot$ will collapse in the far future due to the slow accumulation of iron-56 in their cores. If proton decay does not occur then this is the ultimate fate of about $10^{21}$ stars, approximately one percent of all stars in the observable universe. We present calculations of the internal structure of black dwarfs with iron cores as a model for progenitors. From pycnonuclear fusion rates we estimate their lifetime and thus delay time to be $10^{1100}$ years. We speculate that high mass black dwarf supernovae resemble accretion induced collapse of O/Ne/Mg white dwarfs while later low mass transients will be similar to stripped-envelope core-collapse supernova, and may be the last interesting astrophysical transients to occur prior to heat death.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

摘要：

英文摘要：

相关论文