论文标题
黑洞中子恒星聚结：中子星旋转对喷射发射和动力喷射质量的影响
Black hole-neutron star coalescence: effects of the neutron star spin on jet launching and dynamical ejecta mass
论文作者
论文摘要
黑洞中的星星（BHNS）合并被认为是带有一致电磁（EM）对应物的重力波（GWS）的来源。为了进一步探测这些系统是否是短伽马射线爆发（SGRB）和Kilonovae的可行祖细胞，以及与Ligo/Pirgo候选BHNS GW事件相关的（缺乏）EM如何使用（缺乏）EM来促进参数估算，我们研究了BHNS Mergers中子星的影响。使用BHNS的动态时空磁流体动力学模拟，最初是在半圆形轨道上的，我们调查了BH旋转不同的配置（$ a _ {\ rm bh}/m _ {\ rm bh} ns} = -0.17，\，0，\，0.23 $和$ 0.33 $）和二进制质量比（$ q \ equiv m _ {\ rm bh}：m _ {\ rm ns} = 3：1 $ and $ 5：1 $）。我们发现的一般趋势是，增加NS训练旋转会增加积聚盘的其余质量到残留的黑洞，以及动态弹出的物质的其余质量。到了时间〜$Δt\ sim 3500-5500M \ sim 88-138（m _ {\ rm ns} /1.4m_ \ odot）\，\ rm MS $，峰值引力波振幅（峰值引力波振幅），一种磁性的喷气式飞机仅以$ q = 3：1 $ $ q = 3：1 $ n n s n s n s n s n s n s spine启动。喷气机的寿命[$ΔT\ sim 0.5-0.8（m _ {\ rm ns} /1.4 m_ \ odot）\，\ rm s $]及其出发的发光度[$ l _ {\ rm poyn} Blandford-Znajek机制的典型SGRBS亮度和期望。到我们终止模拟时，我们还没有观察到我们考虑的其他系统的流出或大规模磁场准则。动态弹出物质的质量范围为$ 10^{ - 4.5} -10^{ - 2}〜（m _ {\ rm ns} /1.4m_ \ odot）m_ \ odot $，可以用峰值隆隆量度的峰值为kilonovae供电kilonovae pavice kilonovae peake kilOnovae $ lo _ { ERG/s带有上升时间$ \ lyssim 6.5 \，\ rm h $，并可能通过LSST检测到。
Black hole-neutron star (BHNS) mergers are thought to be sources of gravitational waves (GWs) with coincident electromagnetic (EM) counterparts. To further probe whether these systems are viable progenitors of short gamma-ray bursts (sGRBs) and kilonovae, and how one may use (the lack of) EM counterparts associated with LIGO/Virgo candidate BHNS GW events to sharpen parameter estimation, we study the impact of neutron star spin in BHNS mergers. Using dynamical spacetime magnetohydrodynamic simulations of BHNSs initially on a quasicircular orbit, we survey configurations that differ in the BH spin ($a_{\rm BH}/M_{\rm BH}=0$ and $0.75$), the NS spin ($a_{\rm NS}/M_{\rm NS}=-0.17,\,0,\,0.23$ and $0.33$), and the binary mass ratio ($q\equiv M_{\rm BH}:M_{\rm NS}=3:1$ and $5:1$). The general trend we find is that increasing the NS prograde spin increases both the rest mass of the accretion disk onto the remnant black hole, and the rest mass of dynamically ejected matter. By a time~$Δt\sim 3500-5500M\sim 88-138(M_{\rm NS}/1.4M_\odot)\,\rm ms$ after the peak gravitational wave amplitude, a magnetically--driven jet is launched only for $q=3:1$ regardless of the initial NS spin. The lifetime of the jets [$Δt\sim 0.5-0.8(M_{\rm NS}/1.4 M_\odot)\,\rm s$] and their outgoing Poynting luminosity [$L_{\rm Poyn}\sim 10^{51.5\pm 0.5}\,\rm erg/s$] are consistent with typical sGRBs luminosities and expectations from the Blandford-Znajek mechanism. By the time we terminate our simulations, we do not observe either an outflow or a large-scale magnetic field collimation for the other systems we considered. The mass range of dynamically ejected matter is $10^{-4.5}-10^{-2}~(M_{\rm NS}/1.4M_\odot)M_\odot$, which can power kilonovae with peak bolometric luminosities $L_{\rm knova}\sim 10^{40}-10^{41.4}$ erg/s with rise times $\lesssim 6.5\,\rm h$ and potentially detectable by the LSST.
