论文标题
在稀有的核心塌陷中，行星星云内
On rare core collapse supernovae inside planetary nebulae
论文作者
论文摘要
我们使用白矮人（WD） - 中子星（NS）二进制系统的反向形成的MESA进行模拟，其中WD在NS之前形成。我们得出的结论是，只有当第三颗星形成PN时，核心塌陷超新星（CCSN）爆炸可能发生在行星星云（PN）内。在此WD-NS反向二元演化中，主要恒星将质量进化并转移到次级恒星，形成PN，并留下WD残留物。如果质量转移在发展氦芯之前将次级恒星带来质量> 8mo的质量，并且如果次级在发展大量的氦芯之前不会遭受增强的质量损失，例如，通过质量转移，它将像CCSN一样爆炸，并留下了NS NS ns ns remnant。从主要的PN形成到次级爆炸的时间段> 10^6年。到那时，PN长期已经分散到星际介质中。在具有几乎相等的质量成分的二进制系统中，第一个质量转移发作发生在次级恒星发展出氦芯，并结束其生命形成PN和WD。 PN内部CCSN的形成（CCSNIP）需要第三颗星的存在。第三颗恒星的巨大应比次要恒星少，但不超过几次0.01mo。我们估计CCSNIP的速率是所有CCSNE的速率〜10^{ - 4}倍。
We conduct simulations using MESA of the reverse formation of a white dwarf (WD)-neutron star (NS) binary system in which the WD forms before the NS. We conclude that a core collapse supernova (CCSN) explosion might occur inside a planetary nebula (PN) only if a third star forms the PN. In this WD-NS reverse binary evolution, the primary star evolves and transfers mass to the secondary star, forms a PN, and leaves a WD remnant. If the mass-transfer brings the secondary star to have a mass of >8Mo before it develops a helium core, and if the secondary does not suffer an enhanced mass-loss before it develops a massive helium core, e.g., by mass-transfer, it explodes as a CCSN and leaves a NS remnant. The time period from the formation of the PN by the primary to the explosion of the secondary is >10^6 year. By that time the PN has long dispersed into the interstellar medium. In a binary system with nearly equal mass components, the first mass-transfer episode takes place after the secondary star has developed a helium core and it ends its life forming a PN and a WD. The formation of a CCSN inside a PN (CCSNIP) requires the presence of a third star. The third star should be less massive than the secondary star but by no more than few times 0.01Mo. We estimate that the rate of CCSNIP is ~10^{-4} times the rate of all CCSNe.
