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Exploring the sensitivity of gravitational wave detectors to neutron star physics

Martynov, Denis and Miao, Haixing and Yang, Huan and Hernandez Vivanco, Francisco and Thrane, Eric and Smith, Rory and Lasky, Paul and East, William E. and Adhikari, Rana and Bauswein, Andreas and Brooks, Aidan and Chen, Yanbei and Corbitt, Thomas and Freise, Andreas and Grote, Hartmut and Levin, Yuri and Zhao, Chunnong and Vecchio, Alberto (2019) Exploring the sensitivity of gravitational wave detectors to neutron star physics. Physical Review D, 99 (10). Art. No. 102004. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20190531-091629833

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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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/physrevd.99.102004DOIArticle
https://arxiv.org/abs/1901.03885arXivDiscussion Paper
ORCID:
AuthorORCID
Miao, Haixing0000-0003-2879-5821
Hernandez Vivanco, Francisco0000-0002-1942-7608
Thrane, Eric 0000-0002-4418-3895
Lasky, Paul0000-0003-3763-1386
East, William E.0000-0002-9017-6215
Adhikari, Rana0000-0002-5731-5076
Bauswein, Andreas0000-0001-6798-3572
Brooks, Aidan0000-0003-4295-792X
Corbitt, Thomas0000-0002-5520-8541
Freise, Andreas0000-0001-6586-9901
Zhao, Chunnong0000-0001-5825-2401
Vecchio, Alberto0000-0002-6254-1617
Additional Information:© 2019 American Physical Society. (Received 15 January 2019; published 31 May 2019) We would like to thank members of the LSC AIC, MQM, and QN groups for fruitful discussions and Valery Frolov for reviewing the paper during the internal LIGO review. We acknowledge the support of the National Science Foundation and the LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative Agreement No. PHY-0757058. D. M. and H. M. acknowledge the support of the Institute for Gravitational Wave Astronomy at University of Birmingham. H. M. is supported by UK STFC Ernest Rutherford Fellowship (Grant No. ST/M005844/11). H. Y. is supported by the Natural Sciences and Engineering Research Council of Canada. This research was supported in part by Perimeter Institute for Theoretical Physics. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research and Innovation. A. B. acknowledges support by the European Research Council under the European Unions Horizon 2020 research and innovation programme under Grant No. 759253 and the Klaus-Tschira Foundation. This work is supported through Australian Research Council (ARC) Centre of Excellence CE170100004. E. T. is supported through ARC Future Fellowship FT150100281. P. D. L. is supported through ARC Future Fellowship No. FT160100112 and ARC Discovery Project No. DP180103155.
Group:LIGO
Funders:
Funding AgencyGrant Number
LIGO LaboratoryUNSPECIFIED
NSFPHY-0757058
University of BirminghamUNSPECIFIED
Science and Technology Facilities Council (STFC)ST/M005844/11
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Perimeter Institute for Theoretical PhysicsUNSPECIFIED
Industry CanadaUNSPECIFIED
Ontario Ministry of Research and InnovationUNSPECIFIED
European Research Council (ERC)759253
Klaus Tschira FoundationUNSPECIFIED
Australian Research CouncilCE170100004
Australian Research CouncilFT150100281
Australian Research CouncilFT160100112
Australian Research CouncilDP180103155
Issue or Number:10
Record Number:CaltechAUTHORS:20190531-091629833
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190531-091629833
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95965
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:31 May 2019 17:06
Last Modified:03 Oct 2019 21:18

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