期刊
PHYSICAL REVIEW D
卷 99, 期 10, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.99.102004
关键词
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资金
- National Science Foundation
- LIGO Laboratory
- National Science Foundation [PHY-0757058]
- Institute for Gravitational Wave Astronomy at University of Birmingham
- UK STFC Ernest Rutherford Fellowship [ST/M005844/11]
- Natural Sciences and Engineering Research Council of Canada
- Perimeter Institute for Theoretical Physics
- Government of Canada through Industry Canada
- Province of Ontario through the Ministry of Research and Innovation
- European Research Council under the European Unions Horizon 2020 research and innovation programme [759253]
- Klaus-Tschira Foundation
- Australian Research Council (ARC) Centre of Excellence [CE170100004]
- ARC Future Fellowship [FT150100281, FT160100112]
- ARC Discovery Project [DP180103155]
- STFC [ST/I006269/1, ST/N000633/1, ST/N000072/1, ST/J00166X/1, ST/H002006/1, ST/S000305/1, ST/K000845/1, PPA/G/S/2002/00652, ST/M005844/1] Funding Source: UKRI
The physics of neutron stars can be studied with gravitational waves emitted from coalescing binary systems. Tidal effects become significant during the last few orbits and can be visible in the gravitational wave spectrum above 500 Hz. After the merger, the neutron star remnant oscillates at frequencies above 1 kHz and can collapse into a black hole. Gravitational wave detectors with a sensitivity of similar or equal to 10(-24) strain/root Hz at 2-4 kHz can observe these oscillations from a source which is approximately 100 Mpc away. The current observatories, such as LIGO and Virgo, are limited by shot noise at high frequencies and have a sensitivity of greater than or equal to 2 x 10(-23) strain/root Hz at 3 kHz. In this paper, we propose an optical configuration of gravitational wave detectors, which can be set up in present facilities using the current interferometer topology. This scheme has the potential to reach 7 x 10(-25) strain/root Hz at 2.5 kHz without compromising the detector sensitivity to black hole binaries. We argue that the proposed instruments have the potential to detect similar amount of postmerger neutron star oscillations as the next generation detectors, such as Cosmic Explorer and Einstein Telescope. We also optimize the arm length of the future detectors for neutron star physics and find that the optimal arm length is approximate to 20 km. These instruments have the potential to observe neutron star postmerger oscillations at a rate of approximately 30 events per year with a signal-to-noise ratio of 5 or more.
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