Diagnosing the remnants of binary neutron star merger from GW170817/GRB170817A event
| Autor: | Hou-Jun Lü, En-Wei Liang, Wei-Hua Lei, Lin Lan, Jared Rice, Jun Shen |
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| Rok vydání: | 2019 |
| Předmět: |
Physics
High Energy Astrophysical Phenomena (astro-ph.HE) 010308 nuclear & particles physics Gravitational wave FOS: Physical sciences Astronomy and Astrophysics Astrophysics Magnetar 01 natural sciences Accretion (astrophysics) Afterglow Black hole Neutron star High Energy Physics - Phenomenology High Energy Physics - Phenomenology (hep-ph) Space and Planetary Science 0103 physical sciences Differential rotation Gamma-ray burst Astrophysics - High Energy Astrophysical Phenomena 010303 astronomy & astrophysics |
| DOI: | 10.48550/arxiv.1904.11133 |
| Popis: | 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. Comment: 7 pages, 2 figures. Accepted for publication in MNRAS |
| Databáze: | OpenAIRE |
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