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Tidal disruption as a probe for supermassive black hole binaries

Published online by Cambridge University Press:  07 March 2016

Shuo Li ,
Fukun Liu ,
Peter Berczik  and
Rainer Spurzem
Shuo Li
Affiliation:
National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing, China email: [email protected]
Fukun Liu
Affiliation:
Astronomy Department, Peking University, 100871 Beijing, China Kavli Institute for Astronomy and Astrophysics, Peking University, 100871 Beijing, China
Peter Berczik
Affiliation:
National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing, China email: [email protected] Astronomisches Rechen-Institut, Zentrum für Astronomie, Universität Heidelberg, Mönchhofstr. 12-14, D-69120 Heidelberg, Germany Main Astronomical Observatory, National Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho Street, 03680 Kyiv, Ukraine
Rainer Spurzem
Affiliation:
National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing, China email: [email protected] Astronomisches Rechen-Institut, Zentrum für Astronomie, Universität Heidelberg, Mönchhofstr. 12-14, D-69120 Heidelberg, Germany Kavli Institute for Astronomy and Astrophysics, Peking University, 100871 Beijing, China
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Abstract

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Supermassive black hole binaries (SMBHBs) are the products of frequent galaxy mergers. It is very hard to be detected in quiescent galaxy. By using one million particle direct N-body simulations on special many-core hardware (GPU cluster), we study the dynamical co-evolution of SMBHB and its surrounding stars, specially focusing on the evolution of stellar tidal disruption event (TDE) rates before and after the coalescence of the SMBHB. We find a boosted TDE rate during the merger of the galaxies. After the coalescence of two supermassive black holes (SMBHs), the post-merger SMBH can get a kick velocity due to the anisotropic GW radiations. Our results about the recoiling SMBH, which oscillates around galactic center, show that most of TDEs are contributed by unbound stars when the SMBH passing through galactic center. In addition, the TDE light curve in SMBHB system is significantly different from the curve for single SMBH, which can be used to identify the SMBHB.

Keywords

galaxies: evolutiongalaxies: kinematics and dynamicsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S312: Star Clusters and Black Holes in Galaxies across Cosmic Time , August 2014 , pp. 43 - 47
Copyright
Copyright © International Astronomical Union 2016 

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