Accelerated orbital decay of supermassive black hole binaries in merging nuclear star clusters. Issue 3 (13th February 2020)

• Record Type: Journal Article
• Authors: Ogiya, Go; Hahn, Oliver; Mingarelli, Chiara M F; Volonteri, Marta
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 493:Issue 3(2020)
• Page Start: 3676
• Page End: 3689
• Publication Date: 2020-02-13
• Subjects: black hole physics -- gravitational waves -- methods: numerical -- galaxies: kinematics and dynamics -- galaxies: star clusters: general; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa444
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The coalescence of supermassive black holes (SMBHs) should generate the strongest sources of gravitational waves (GWs) in the Universe. However, the dynamics of their coalescence is the subject of much debate. In this study, we use a suite of N -body simulations to follow the merger of two nuclear star clusters (NSCs), each hosting an SMBH in their centre. We find that the presence of distinct star clusters around each SMBH has important consequences for the dynamical evolution of the SMBH binary: (i) The separation between the SMBHs decreases by a few orders of magnitude in the first few Myrs by the combined effects of dynamical friction and a drag force caused by tidally stripped stars. In fact, this is a significant speedup for equal mass ratio binaries, and becomes extreme for unequal mass ratios, e.g. 1:10 or 1:100, which traditional dynamical friction alone would not permit to bind. (ii) The subsequent binary hardening is driven by the gravitational slingshots between the SMBH binary and stars, and also depends on the mass ratio between the SMBHs. Thus, with this additional drag force, we find that all SMBHs in our suite coalesce within a Hubble time. Given that about 50 per cent of Milky Way-sized galaxies host NSCs, our results are encouraging for upcoming GW observations with the Laser Interferometer Space Antenna – LISA – which will detect SMBH coalescence in the 10 4 –10 7 M⊙ mass range.