论文标题
快速旋转的伽马射线爆发和相关的基洛诺瓦从快速旋转黑洞 - 中子星星合并
Long-duration Gamma-ray Burst and Associated Kilonova Emission from Fast-spinning Black Hole--Neutron Star Mergers
论文作者
论文摘要
在这里，我们收集了三个独特的爆发，GRBS \，060614、211211A和211227A，所有这些都以长持续的主要发射相（ME）相位和重新膨胀的扩展发射（EE）阶段为特征，以研究其观察到的属性，并且作为中子星空孔（NSBH）Mergers的潜在特性和潜在的起源。 NS首发（BH先生）的NSBH合并倾向于包含快速旋转（非旋转）BHS，更容易（几乎）（几乎不）使潮汐破坏发生在（没有）形成电磁信号的情况下。我们发现，NS首发的NSBH合并可以很好地解释这三个GRB的起源，并由此功能支持：（1）他们的X射线MES和EES显示出明显的下后倒下积聚签名，减少为$ \ propto {t}^{-5/3} $，其中可能会说明他们的长期持久。 EES可能是由$ r $ $ process供暖材料的秋季后积聚产生的，该材料预计将在NSBH合并后发生。 （2）这种类型的合并 - 原始长期长期grb的横梁校正的本地事件密度是$ \ natercal {r} _0 \ sim2.4^{+2.3} _ { - 1.3} \，{\ rm {\ rm {\ rm {gpc}}}}与NS成立的NSBH合并一致。 （3）我们对最近高影响事件的EE，Afterglow和Kilonova的详细分析GRB \，211211a表明，它可能是$ \ sim1.23^{+0.06} _ { - 0.06} _ { - 0.07} $ \ sim8.21^{+0.77} _ { - 0.75} \，m _ \ odot $ bh，其对齐的旋转为$χ_ {\ rm {bh}} \ sim0.62 \ sim0.62^{+0.06} {+0.06} _ { - 0.07} _ { - 0.07} $，ns ns ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-ns-n s ns-ns ns-ns-ns-bort。在我之后，长期爆发的爆发爆发，偏高的倒下积聚签名和轴上NSBH的特征通常是明亮的Kilonova。我们估计了O4（O5）中NSBH合并的重力波，GRB和Kilonovae之间的多通电器检测率，为$ \ sim0.1 \，{\ rm {yr}}^{ - 1} { - 1} $（$ \ sim1 \ sim1 \，，{\ rm {\ rm {\ rm {\ rm {\ rm {\ rm {yr {yr}}
Here we collect three unique bursts, GRBs\,060614, 211211A and 211227A, all characterized by a long-duration main emission (ME) phase and a rebrightening extended emission (EE) phase, to study their observed properties and the potential origin as neutron star-black hole (NSBH) mergers. NS-first-born (BH-first-born) NSBH mergers tend to contain fast-spinning (non-spinning) BHs that more easily (hardly) allow tidal disruption to happen with (without) forming electromagnetic signals. We find that NS-first-born NSBH mergers can well interpret the origins of these three GRBs, supported by that: (1) Their X-ray MEs and EEs show unambiguous fall-back accretion signatures, decreasing as $\propto{t}^{-5/3}$, which might account for their long duration. The EEs can result from the fall-back accretion of $r$-process heating materials, predicted to occur after NSBH mergers. (2) The beaming-corrected local event rate density for this type of merger-origin long-duration GRBs is $\mathcal{R}_0\sim2.4^{+2.3}_{-1.3}\,{\rm{Gpc}}^{-3}\,{\rm{yr}}^{-1}$, consistent with that of NS-first-born NSBH mergers. (3) Our detailed analysis on the EE, afterglow and kilonova of the recently high-impact event GRB\,211211A reveals it could be a merger between a $\sim1.23^{+0.06}_{-0.07}\,M_\odot$ NS and a $\sim8.21^{+0.77}_{-0.75}\,M_\odot$ BH with an aligned-spin of $χ_{\rm{BH}}\sim0.62^{+0.06}_{-0.07}$, supporting an NS-first-born NSBH formation channel. Long-duration burst with rebrightening fall-back accretion signature after ME, and bright kilonova might be commonly observed features for on-axis NSBHs. We estimate the multimessenger detection rate between gravitational waves, GRBs and kilonovae from NSBH mergers in O4 (O5) is $\sim0.1\,{\rm{yr}}^{-1}$ ($\sim1\,{\rm{yr}}^{-1}$).
