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Merging of spinning binary black holes in globular clusters

Published online by Cambridge University Press:  20 January 2023

Margarita Sobolenko Open the ORCID record for Margarita Sobolenko [Opens in a new window] ,
Peter Berczik Open the ORCID record for Peter Berczik [Opens in a new window] ,
Manuel Arca Sedda Open the ORCID record for Manuel Arca Sedda [Opens in a new window] ,
Konrad Maliszewski ,
Mirek Giersz Open the ORCID record for Mirek Giersz [Opens in a new window]  and
Rainer Spurzem
Margarita Sobolenko
Affiliation:
Main Astronomical Observatory, National Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho St., 03143 Kyiv, Ukraine email (MS): [email protected]
Peter Berczik
Affiliation:
Main Astronomical Observatory, National Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho St., 03143 Kyiv, Ukraine email (MS): [email protected] Astronomisches Rechen Institut - Zentrum für Astronomie der Universität Heidelberg, Mönchhofstrasse 12-14, D-69120 Heidelberg, Germany Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network (ELKH), MTA Centre of Excellence, Konkoly Thege Miklósút 15-17, 1121 Budapest, Hungary
Manuel Arca Sedda
Affiliation:
Astronomisches Rechen Institut - Zentrum für Astronomie der Universität Heidelberg, Mönchhofstrasse 12-14, D-69120 Heidelberg, Germany
Konrad Maliszewski
Affiliation:
Astronomical Observatory, Warsaw University, al. Ujazdowskie 4, 00-478 Warsaw, Poland
Mirek Giersz
Affiliation:
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
Rainer Spurzem
Affiliation:
Astronomisches Rechen Institut - Zentrum für Astronomie der Universität Heidelberg, Mönchhofstrasse 12-14, D-69120 Heidelberg, Germany Kavli Institute for Astronomy and Astrophysics, Peking University, Yiheyuan Lu 5, Haidian Qu, 100871, Beijing, China
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Abstract

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Based on our current high resolution direct N-body modelling of the Milky Way typical Star Cluster systems dynamical evolution we try to numerically estimate the influence of individual spin values and orientations on gravitational wave (GW) waveforms and observed time-frequency maps during multiple cycles for binary black hole (BBH) mergers. In our up to date N-body dynamical simulations we use the high order relativistic post-Newtonian corrections for the BH binary particles (3.5 post-Newtonian (PN) terms including spin-spin and spin-orbit terms). In the current work, we present the GW waveforms catalogue which covers the large parameter space in mass ratios 0.05 - 0.82 and extreme possible individual spin cases.

Keywords

black hole physicsgravitational wavesmethods: n-body simulations
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 203 - 208
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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