2021年2月
Properties of the remnant disk and the dynamical ejecta produced in low-mass black hole-neutron star mergers
PHYSICAL REVIEW D
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- 巻
- 103
- 号
- 4
- 記述言語
- 英語
- 掲載種別
- DOI
- 10.1103/PhysRevD.103.043007
- 出版者・発行元
- AMER PHYSICAL SOC
We systematically perform numerical-relativity simulations for low-mass black hole-neutron star mergers for the models with seven mass ratios Q = M-BH/M-NS ranging from 1.5 to 4.4, and three neutron-star equations of state, focusing on the properties of matter remaining outside the black hole and ejected dynamically during the merger. We pay particular attention to the dependence on the mass ratio of the binaries. It is found that the rest mass remaining outside the apparent horizon after the merger depends only weakly on the mass ratio for the models with low mass ratios. It is also clarified that the rest mass of the ejecta has a peak at Q similar to 3, and decreases steeply as the mass ratio decreases for the low mass-ratio case. We present a novel analysis method for the behavior of matter during the merger, focusing on the matter distribution in the phase space of specific energy and specific angular momentum. Then we model the matter distribution during and after the merger. Using the result of the analysis, we discuss the properties of the ejecta.
- リンク情報
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- DOI
- https://doi.org/10.1103/PhysRevD.103.043007
- arXiv
- http://arxiv.org/abs/arXiv:2010.02563
- Web of Science
- https://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcAuth=JSTA_CEL&SrcApp=J_Gate_JST&DestLinkType=FullRecord&KeyUT=WOS:000617042600001&DestApp=WOS_CPL
- URL
- http://arxiv.org/abs/2010.02563v1
- URL
- http://arxiv.org/pdf/2010.02563v1 本文へのリンクあり
- ID情報
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- DOI : 10.1103/PhysRevD.103.043007
- ISSN : 2470-0010
- eISSN : 2470-0029
- arXiv ID : arXiv:2010.02563
- Web of Science ID : WOS:000617042600001