Exploring the sensitivity of gravitational wave detectors to neutron star physics

Denis Martynov, Haixing Miao, Huan Yang, Francisco Hernandez Vivanco, Eric Thrane, Rory Smith, Paul Lasky, William E. East, Rana Adhikari, Andreas Bauswein, Aidan Brooks, Yanbei Chen, Thomas Corbitt, Andreas Freise, Hartmut Grote, Yuri Levin, Chunnong Zhao, Alberto Vecchio

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10 Citations (Scopus)

Abstract

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 ≃10-24 strain/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 2×10-23 strain/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 7×10-25 strain/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 ≈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.

Original languageEnglish
Article number102004
Number of pages17
JournalPhysical Review D
Volume99
Issue number10
DOIs
Publication statusPublished - 15 May 2019

Cite this

Martynov, Denis ; Miao, Haixing ; Yang, Huan ; Vivanco, Francisco Hernandez ; Thrane, Eric ; Smith, Rory ; Lasky, Paul ; East, William E. ; Adhikari, Rana ; Bauswein, Andreas ; Brooks, Aidan ; Chen, Yanbei ; Corbitt, Thomas ; Freise, Andreas ; Grote, Hartmut ; Levin, Yuri ; Zhao, Chunnong ; Vecchio, Alberto. / Exploring the sensitivity of gravitational wave detectors to neutron star physics. In: Physical Review D. 2019 ; Vol. 99, No. 10.
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abstract = "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 ≃10-24 strain/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 2×10-23 strain/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 7×10-25 strain/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 ≈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.",
author = "Denis Martynov and Haixing Miao and Huan Yang and Vivanco, {Francisco Hernandez} and Eric Thrane and Rory Smith and Paul Lasky and East, {William E.} and Rana Adhikari and Andreas Bauswein and Aidan Brooks and Yanbei Chen and Thomas Corbitt and Andreas Freise and Hartmut Grote and Yuri Levin and Chunnong Zhao and Alberto Vecchio",
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Martynov, D, Miao, H, Yang, H, Vivanco, FH, Thrane, E, Smith, R, Lasky, P, East, WE, Adhikari, R, Bauswein, A, Brooks, A, Chen, Y, Corbitt, T, Freise, A, Grote, H, Levin, Y, Zhao, C & Vecchio, A 2019, 'Exploring the sensitivity of gravitational wave detectors to neutron star physics', Physical Review D, vol. 99, no. 10, 102004. https://doi.org/10.1103/PhysRevD.99.102004

Exploring the sensitivity of gravitational wave detectors to neutron star physics. / Martynov, Denis; Miao, Haixing; Yang, Huan; Vivanco, Francisco Hernandez; Thrane, Eric; Smith, Rory; Lasky, Paul; East, William E.; Adhikari, Rana; Bauswein, Andreas; Brooks, Aidan; Chen, Yanbei; Corbitt, Thomas; Freise, Andreas; Grote, Hartmut; Levin, Yuri; Zhao, Chunnong; Vecchio, Alberto.

In: Physical Review D, Vol. 99, No. 10, 102004, 15.05.2019.

Research output: Contribution to journalArticleResearchpeer-review

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T1 - Exploring the sensitivity of gravitational wave detectors to neutron star physics

AU - Martynov, Denis

AU - Miao, Haixing

AU - Yang, Huan

AU - Vivanco, Francisco Hernandez

AU - Thrane, Eric

AU - Smith, Rory

AU - Lasky, Paul

AU - East, William E.

AU - Adhikari, Rana

AU - Bauswein, Andreas

AU - Brooks, Aidan

AU - Chen, Yanbei

AU - Corbitt, Thomas

AU - Freise, Andreas

AU - Grote, Hartmut

AU - Levin, Yuri

AU - Zhao, Chunnong

AU - Vecchio, Alberto

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AB - 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 ≃10-24 strain/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 2×10-23 strain/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 7×10-25 strain/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 ≈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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