Simulation of the gravitational wave frequency distribution of neutron star-black hole mergers

doi:10.1088/1674-1056/abff28

中国物理B ›› 2021, Vol. 30 ›› Issue (12): 120401-120401.doi: 10.1088/1674-1056/abff28

Simulation of the gravitational wave frequency distribution of neutron star-black hole mergers

Jianwei Zhang(张见微)^1,2, Chengmin Zhang(张承民)^1,2,†, Di Li(李菂)^1,2,6,‡, Xianghan Cui(崔翔翰)^1,2, Wuming Yang(杨伍明)³, Dehua Wang(王德华)⁴, Yiyan Yang(杨佚沿)⁵, Shaolan Bi(毕少兰)³, and Xianfei Zhang(张先飞)³

1 CAS Key Laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China;
2 University of Chinese Academy of Sciences, Beijing 100049, China;
3 Department of Astronomy, Beijing Normal University, Beijing 100875, China;
4 School of Physics and Electronic Science, Guizhou Normal University, Guiyang 550001, China;
5 School of Physics and Electronic Science, Guizhou Education University, Guiyang 550018, China;
6 NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa

收稿日期:2021-03-15 修回日期:2021-04-23 接受日期:2021-05-08 出版日期:2021-11-15 发布日期:2021-11-15
通讯作者: Chengmin Zhang, Di Li E-mail:zhangcm@bao.ac.cn;dili@nao.cas.cn
基金资助:
Project supported by the National Natural Science Foundation of China (Grant Nos. 11988101, 11773005, U2031203, U1631236, 11703001, U1731238, U1938117, 11725313, and 11721303), the International Partnership Program of Chinese Academy of Sciences (Grant No. 114A11KYSB20160008), and the National Key R&D Program of China (Grant No. 2016YFA0400702), and the Subsidy Project of the National Natural Science Foundation of China (Grant No. 2021GZJ006).

Simulation of the gravitational wave frequency distribution of neutron star-black hole mergers

1 CAS Key Laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China;
2 University of Chinese Academy of Sciences, Beijing 100049, China;
3 Department of Astronomy, Beijing Normal University, Beijing 100875, China;
4 School of Physics and Electronic Science, Guizhou Normal University, Guiyang 550001, China;
5 School of Physics and Electronic Science, Guizhou Education University, Guiyang 550018, China;
6 NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa

Received:2021-03-15 Revised:2021-04-23 Accepted:2021-05-08 Online:2021-11-15 Published:2021-11-15
Contact: Chengmin Zhang, Di Li E-mail:zhangcm@bao.ac.cn;dili@nao.cas.cn
Supported by:
Project supported by the National Natural Science Foundation of China (Grant Nos. 11988101, 11773005, U2031203, U1631236, 11703001, U1731238, U1938117, 11725313, and 11721303), the International Partnership Program of Chinese Academy of Sciences (Grant No. 114A11KYSB20160008), and the National Key R&D Program of China (Grant No. 2016YFA0400702), and the Subsidy Project of the National Natural Science Foundation of China (Grant No. 2021GZJ006).

摘要/Abstract

摘要： LIGO-Virgo has observed the gravitational waves (GWs) from the coalescence of binary black hole (BBH) and binary neutron star (BNS) during O1 and O2, and the ones from NS-BH are expected to be hunted in the operating O3 run. The population properties and mass distribution of NS-BH mergers are poorly understood now, thus researchers simulated their chirp mass ($\mathcal{M}$) distribution by a synthetic model, in which the BHs and NSs were inferred by LIGO-Virgo (O1/O2), and obtained the values in the range of $2.1M_{\odot}<\mathcal{M}<7.3M_{\odot}$. In this paper, we further simulate the GW frequency ($f_{\scriptscriptstyle {\rm GW}}$) distribution of NS-BH mergers by the above-stated synthetic model, with a basic binary system model through the Monte Carlo method. Our results predict that the median with 90% credible intervals is $165_{-64}^{+475}$~Hz in the case of Schwarzschild BH when the system just before merger, and this GW frequency is expected to increase several times in the merger stage, which is lying in the frequency band of LIGO-Virgo, i.e., about 15 ~Hz to a few kHz. Our results provide an important reference for hunting the NS-BH mergers by the on-going O3 run of LIGO-Virgo.

关键词: gravitational waves, statistical methods, neutron stars, black holes

Abstract: LIGO-Virgo has observed the gravitational waves (GWs) from the coalescence of binary black hole (BBH) and binary neutron star (BNS) during O1 and O2, and the ones from NS-BH are expected to be hunted in the operating O3 run. The population properties and mass distribution of NS-BH mergers are poorly understood now, thus researchers simulated their chirp mass ($\mathcal{M}$) distribution by a synthetic model, in which the BHs and NSs were inferred by LIGO-Virgo (O1/O2), and obtained the values in the range of $2.1M_{\odot}<\mathcal{M}<7.3M_{\odot}$. In this paper, we further simulate the GW frequency ($f_{\scriptscriptstyle {\rm GW}}$) distribution of NS-BH mergers by the above-stated synthetic model, with a basic binary system model through the Monte Carlo method. Our results predict that the median with 90% credible intervals is $165_{-64}^{+475}$~Hz in the case of Schwarzschild BH when the system just before merger, and this GW frequency is expected to increase several times in the merger stage, which is lying in the frequency band of LIGO-Virgo, i.e., about 15 ~Hz to a few kHz. Our results provide an important reference for hunting the NS-BH mergers by the on-going O3 run of LIGO-Virgo.

Key words: gravitational waves, statistical methods, neutron stars, black holes

中图分类号: (Gravitational waves)

04.30.-w

02.70.Rr (General statistical methods) 97.60.Jd (Neutron stars) 97.60.Lf (Black holes)

Jianwei Zhang(张见微), Chengmin Zhang(张承民), Di Li(李菂), Xianghan Cui(崔翔翰), Wuming Yang(杨伍明), Dehua Wang(王德华), Yiyan Yang(杨佚沿), Shaolan Bi(毕少兰), and Xianfei Zhang(张先飞). Simulation of the gravitational wave frequency distribution of neutron star-black hole mergers[J]. 中国物理B, 2021, 30(12): 120401-120401.

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Simulation of the gravitational wave frequency distribution of neutron star-black hole mergers

Simulation of the gravitational wave frequency distribution of neutron star-black hole mergers

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