论文标题
黑矮人超新星未来
Black Dwarf Supernova in the Far Future
论文作者
论文摘要
在恒星形成停止后很久的未来，宇宙将被稀疏的堕落残余物（主要是白矮人）所占据，尽管他们的最终命运是一个悬而未决的问题。这些白色矮人会冷却并冷冻固体成黑矮人，而pycnonaclear融合会慢慢将其成分加工为铁-56。但是，由于电子的下降，这些恒星的Chandrasekhar极限将减少，最终将低于最大的黑矮星。因此，由于铁-56在其内核中的缓慢积累，隔离的质量大于$ \ sim 1.2 m_ \ odot $的隔离矮星将在远的未来崩溃。如果未发生质子衰减，那么这是约$ 10^{21} $星星的最终命运，大约是可观察到的宇宙中全恒星的百分之一。我们介绍了用铁芯作为祖细胞模型的黑矮人的内部结构的计算。从pycnonaclear融合率开始，我们估计它们的寿命，因此延迟时间为$ 10^{1100} $年。我们推测，高质量的黑矮人超新星类似于o/ne/mg白色矮人的塌陷，而后来的低质量瞬变将与剥离的eNVELOPE核心 - 循环崩溃的超新星相似，并且可能是最后一次有趣的天体物理瞬变，发生在热死亡之前。
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.
