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Exploring the sensitivity of gravitational wave detectors to neutron star physics

Denis Martynov1,*, Haixing Miao1, Huan Yang2,3, Francisco Hernandez Vivanco4,5, Eric Thrane4,5, Rory Smith4,5, Paul Lasky4,5, William E. East2, Rana Adhikari6 et al.

Andreas Bauswein7,8, Aidan Brooks6, Yanbei Chen6, Thomas Corbitt9, Andreas Freise1, Hartmut Grote10, Yuri Levin11,12, Chunnong Zhao13,5, and Alberto Vecchio1

  • 1School of Physics and Astronomy, and Institute of Gravitational Wave Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, United Kingdom
  • 2Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L2Y5, Canada
  • 3University of Guelph, Guelph, Ontario N2L3G1, Canada
  • 4School of Physics and Astronomy, Monash University, Victoria, Clayton 3800, Australia
  • 5OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery, Victoria, Clayton 3800, Australia
  • 6LIGO, California Institute of Technology, Pasadena, California 91125, USA
  • 7GSI Helmholtzzentrum fr Schwerionenforschung, Planckstrae 1, 64291 Darmstadt, Germany
  • 8Heidelberg Institute for Theoretical Studies, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany
  • 9Department of Physics & Astronomy, Louisiana State University, Baton Rouge, Louisiana 70803, USA
  • 10School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, United Kingdom
  • 11Physics Department and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA
  • 12Center for Computational Astrophysics, Flatiron Institute, New York, New York 10010, USA
  • 13ARC Centre of Excellence for Gravitational Wave Discovery, The University of Western Australia, Crawley, Western Australia 6009, Australia

  • *Corresponding author. dmartynov@star.sr.bham.ac.uk
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Phys. Rev. D 99, 102004 – Published 31 May, 2019

DOI: https://doi.org/10.1103/PhysRevD.99.102004

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.

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Phys. Rev. D 99, 102004– Published 31 May, 2019
  • Received 15 January 2019
Article part of CHORUS
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