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arXiv 1505.02809astro-ph.HE
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双星驱动超新星产生的中子星-黑洞双星

On the Neutron Star-Black Hole Binaries Produced by Binary-driven-Hypernovae

C. L. Fryer, F. G. Oliveira, J. A. Rueda, R. Ruffini

备注：
Accepted for publication in Physical Review Letters
发表信息：
Phys. Rev. Lett. 115, 231102 (2015)
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摘要：

在诱导引力坍缩（IGC）范式中，引入双星驱动超超新星（BdHNe）解释了与Ic型超新星（SNe）有关的高能（$E_{\rm iso}\gtrsim 10^{52}$ ~erg）长伽马射线暴（GRB）。它的前身是一个紧密的双星，由一个碳氧（CO）核心和一个中子星（NS）伴星组成，是新提出的“超剥离”双星的一个子类。当CO核心坍缩时，CO-NS短周期轨道导致NS从SN喷出物中吸积适当的物质，最终导致其坍缩为黑洞（BH）并产生GRB。这些紧密的双星演化通过SN爆炸非常不同的人口合成计算研究的紧凑型双星。首先，NS伴星的超临界吸积改变了双星的质量和动量。第二，因为爆炸的时间尺度与轨道周期相同，所以不能假设物质抛射是瞬时的。这极大地影响了双星系统在SN之后的命运。最后，当吸积的NS犁过SN喷出物时产生的弓形激波传递角动量，制动轨道。即使在爆炸中损失了很大一部分双星质量（远高于规范的50%极限），这些系统仍然保持束缚，即使是大的反冲也不太可能使系统脱离束缚。事实上，BdHNe产生了一个新的NS-BH双星家族，在目前的人口合成分析中没有考虑到，尽管它们可能很罕见，但近100%的结合率意味着它们可能在紧凑的合并率中发挥重要作用，这对引力波（GW）很重要，反过来，可以产生一类新的超短GRB。

英文摘要：

Binary-driven-hypernovae (BdHNe) within the induced gravitational collapse (IGC) paradigm have been introduced to explain energetic ($E_{\rm iso}\gtrsim 10^{52}$~erg), long gamma-ray bursts (GRBs) associated with type Ic supernovae (SNe). The progenitor is a tight binary composed of a carbon-oxygen (CO) core and a neutron star (NS) companion, a subclass of the newly proposed "ultra-stripped" binaries. The CO-NS short-period orbit causes the NS to accrete appriciable matter from the SN ejecta when the CO core collapses, ultimately causing it to collapse to a black hole (BH) and producing a GRB. These tight binaries evolve through the SN explosion very differently than compact binaries studied in population synthesis calculations. First, the hypercritical accretion onto the NS companion alters both the mass and momentum of the binary. Second, because the explosion timescale is on par with the orbital period, the mass ejection can not be assumed to be instantaneous. This dramatically affects the post-SN fate of the binary. Finally, the bow shock created as the accreting NS plows through the SN ejecta transfers angular momentum, braking the orbit. These systems remain bound even if a large fraction of the binary mass is lost in the explosion (well above the canonical 50\% limit), and even large kicks are unlikely to unbind the system. Indeed, BdHNe produce a new family of NS-BH binaries unaccounted for in current population synthesis analyses and, although they may be rare, the fact that nearly 100\% remain bound implies they may play an important role in the compact merger rate, important for gravitational waves (GWs) that, in turn, can produce a new class of ultrashort GRBs.

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