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Post-Newtonian dynamics in dense star clusters: Binary black holes in the LISA band

Kyle Kremer1,2,*, Carl L. Rodriguez3, Pau Amaro-Seoane4, Katelyn Breivik5, Sourav Chatterjee2,6, Michael L. Katz1,2, Shane L. Larson1,2, Frederic A. Rasio1,2, Johan Samsing7 et al.

Claire S. Ye1,2 and Michael Zevin1,2

  • 1Department of Physics & Astronomy, Northwestern University, Evanston, Illinois 60202, USA
  • 2Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Evanston, Illinois 60202, USA
  • 3Pappalardo Fellow; MIT-Kavli Institute for Astrophysics and Space Research, Cambridge, Massachusetts 02139, USA
  • 4Institute of Space Sciences (ICE, CSIC) & Institut d’Estudis Espacials de Catalunya (IEEC) at Campus UAB, Carrer de Can Magrans s/n 08193 Barcelona, Spain Institute of Applied Mathematics, Academy of Mathematics and Systems Science, CAS, Beijing 100190, China Kavli Institute for Astronomy and Astrophysics, Beijing 100871, China
  • 5Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Ontario M5S 3H8, Canada
  • 6Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India
  • 7Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA

  • *kremer@u.northwestern.edu
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Phys. Rev. D 99, 063003 – Published 6 March, 2019

DOI: https://doi.org/10.1103/PhysRevD.99.063003

Abstract

The dynamical processing of black holes in the dense cores of globular clusters (GCs) makes them efficient factories for producing binary black holes (BBHs). Here we explore the population of BBHs that form dynamically in GCs and may be observable at mHz frequencies or higher with the future space-based gravitational-wave observatory LISA. We use our Monte Carlo stellar dynamics code, which includes gravitational radiation reaction effects for all BH encounters. By creating a representative local universe of GCs, we show that up to dozens of these systems may be resolvable by LISA. Approximately one-third of these binaries will have measurable eccentricities (e>10−3) in the LISA band, and a small number (≲5) may evolve from the LISA band to the LIGO band during the LISA mission.

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Phys. Rev. D 99, 063003– Published 6 March, 2019
  • Received 28 November 2018
Article part of CHORUS
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