Diagnosing the remnants of binary neutron star merger from GW170817/GRB170817A event
Diagnosing the remnants of binary neutron star merger from GW170817/GRB170817A event
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诊断 GW170817/GRB170817A 事件双中子星合并的残余物
DOI：
10.1093/mnras/stz1155
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发表时间：
2019-04
影响因子：
4.8
通讯作者：
Liang En-Wei
中科院分区：
文献类型：
--
作者：
Lu Hou-Jun;Shen Jun;Lan Lin;Rice Jared;Lei Wei-Hua;Liang En-Wei
GW170817/GRB 170817A事件是通过对其引力波辐射和多波长电磁辐射的成功联合观测发现的，是两颗中子星合并的第一个明确的“证据”。然而，合并的剩余部分仍然未知。Piro等人最近声称GRB 170817A的x射线变异性不显著。通过系统地比较GRB 170817A余辉的变异性和GRB余辉中的x射线耀斑的变异性，我们发现这种x射线变异性似乎与GRB余辉中的x射线耀斑具有相似的统计相关性。我们进一步研究了几种可能的合并产物情景，看看它们是否能产生GRB 170817A中观测到的x射线变异性。第一种情况需要一颗稳定的磁星作为中央引擎，通过差速旋转或后退吸积到NS产生后来的x射线变异性。第二种情况需要一个黑洞作为中央引擎，并进行回退吸积过程。最后一种情况是一个具有长寿命超大质量NS的中央引擎。我们发现前两种情况很难产生后一种x射线变异性，这要么需要不切实际的NS磁场，要么需要非常大的恒星包层和非常长的吸积时间尺度。然而，第三种情况似乎与观测结果一致，并且后来的x射线变率可以由磁层产生，磁层在NS坍缩后以$B_p\in(3.6, 13.5)\times10^{13}$ G被驱逐。
The event GW170817/GRB 170817A, discovered via the successful joint observation of its gravitational wave radiation and its multi-wavelength electromagnetic counterparts, was the first definite "smoking-gun" from the merger of two neutron stars (NSs). However, the remnant of the merger remains unknown. Piro et al. recently claimed that a low-significance X-ray variability in GRB 170817A. By systematically comparing the properties of variability in the afterglow of GRB 170817A and X-ray flares in GRB afterglows, we find that this X-ray variability seems to share similar statistical correlations with X-ray flares in GRB afterglows. We further investigate several possible merger product scenarios to see whether they can produce the observed X-ray variability in GRB 170817A. The first scenario invokes a stable magnetar as the central engine producing the later X-ray variability via differential rotation or fall-back accretion onto the NS. The second scenario invokes a black hole as the central engine with a fall-back accretion process. The final scenario is a central engine with a long-lived supra-massive NS. We find that the first two scenarios have difficulty producing the later X-ray variability, which requires either an impractical NS magnetic field or an extraordinarily large stellar envelope and an extremely long accretion timescale. However, the third scenario seems to be consistent with observations, and the later X-ray variability can be produced by the magnetosphere which is expelled following the collapse of the NS with a $B_p\in(3.6, 13.5)\times10^{13}$ G.
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影响因子：
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作者：
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通讯作者：
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影响因子：
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作者：
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通讯作者：
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影响因子：
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