Detecting short-term gravitational waves from post-merger hyper-massive neutron stars with a kilohertz detector

doi:10.1088/1674-1056/ad5320

中国物理B ›› 2024, Vol. 33 ›› Issue (8): 80401-080401.doi: 10.1088/1674-1056/ad5320

Detecting short-term gravitational waves from post-merger hyper-massive neutron stars with a kilohertz detector

Yikang Chen(陈奕康)^1,2 and Zong-Hong Zhu(朱宗宏)^1,2,†

1 Institute for Frontier in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China;
2 Department of Astronomy, Beijing Normal University, Beijing 100875, China

收稿日期:2024-03-14 修回日期:2024-05-12 出版日期:2024-08-15 发布日期:2024-07-23
通讯作者: Zong-Hong Zhu E-mail:zhuzh@bnu.edu.cn
基金资助:
This project was supported by the National Natural Science Foundation of China (Grant Nos. 12021003, 11920101003, and 11633001), and the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDB23000000).

Detecting short-term gravitational waves from post-merger hyper-massive neutron stars with a kilohertz detector

Yikang Chen(陈奕康)^1,2 and Zong-Hong Zhu(朱宗宏)^1,2,†

1 Institute for Frontier in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China;
2 Department of Astronomy, Beijing Normal University, Beijing 100875, China

Received:2024-03-14 Revised:2024-05-12 Online:2024-08-15 Published:2024-07-23
Contact: Zong-Hong Zhu E-mail:zhuzh@bnu.edu.cn
Supported by:
This project was supported by the National Natural Science Foundation of China (Grant Nos. 12021003, 11920101003, and 11633001), and the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDB23000000).

摘要/Abstract

摘要： Gravitational waves emanating from binary neutron star inspirals, alongside electromagnetic transients resulting from the aftermath of the GW170817 merger, have been successfully detected. However, the intricate post-merger dynamics that bridge these two sets of observables remain enigmatic. This includes if, and when, the post-merger remnant star collapses to a black hole, and what are the necessary conditions to power a short gamma-ray burst, and other observed electromagnetic counterparts. Our focus is on the detection of gravitational wave (GW) emissions from hyper-massive neutron stars (NSs) formed through binary neutron star (BNS) mergers. Utilizing several kilohertz GW detectors, we simulate BNS mergers within the detection limits of LIGO-Virgo-KARGA O4. Our objective is to ascertain the fraction of simulated sources that may emit detectable post-merger GW signals. For kilohertz detectors equipped with a new cavity design, we estimate that approximately 1.1%-32% of sources would emit a detectable post-merger GW signal. This fraction is contingent on the mass converted into gravitational wave energy, ranging from $0.01M_{\rm sun}$ to $0.1M_{\rm sun}$. Furthermore, by evaluating other well-regarded proposed kilohertz GW detectors, we anticipate that the fraction can increase to as much as 2.1%-61% under optimal performance conditions.

关键词: neutron star mergers, gravitational waves

Abstract: Gravitational waves emanating from binary neutron star inspirals, alongside electromagnetic transients resulting from the aftermath of the GW170817 merger, have been successfully detected. However, the intricate post-merger dynamics that bridge these two sets of observables remain enigmatic. This includes if, and when, the post-merger remnant star collapses to a black hole, and what are the necessary conditions to power a short gamma-ray burst, and other observed electromagnetic counterparts. Our focus is on the detection of gravitational wave (GW) emissions from hyper-massive neutron stars (NSs) formed through binary neutron star (BNS) mergers. Utilizing several kilohertz GW detectors, we simulate BNS mergers within the detection limits of LIGO-Virgo-KARGA O4. Our objective is to ascertain the fraction of simulated sources that may emit detectable post-merger GW signals. For kilohertz detectors equipped with a new cavity design, we estimate that approximately 1.1%-32% of sources would emit a detectable post-merger GW signal. This fraction is contingent on the mass converted into gravitational wave energy, ranging from $0.01M_{\rm sun}$ to $0.1M_{\rm sun}$. Furthermore, by evaluating other well-regarded proposed kilohertz GW detectors, we anticipate that the fraction can increase to as much as 2.1%-61% under optimal performance conditions.

Key words: neutron star mergers, gravitational waves

中图分类号: (Gravitational waves)

04.30.-w

04.80.Nn (Gravitational wave detectors and experiments) 97.60.Jd (Neutron stars)

Yikang Chen(陈奕康) and Zong-Hong Zhu(朱宗宏). Detecting short-term gravitational waves from post-merger hyper-massive neutron stars with a kilohertz detector[J]. 中国物理B, 2024, 33(8): 80401-080401.

Yikang Chen(陈奕康) and Zong-Hong Zhu(朱宗宏). Detecting short-term gravitational waves from post-merger hyper-massive neutron stars with a kilohertz detector[J]. Chin. Phys. B, 2024, 33(8): 80401-080401.

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Detecting short-term gravitational waves from post-merger hyper-massive neutron stars with a kilohertz detector

Detecting short-term gravitational waves from post-merger hyper-massive neutron stars with a kilohertz detector

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