scholarly journals Massive black hole binaries from runaway collisions: the impact of metallicity

2016 ◽  
Vol 459 (4) ◽  
pp. 3432-3446 ◽  
Author(s):  
Michela Mapelli
Keyword(s):  
Black Hole ◽  
Massive Black Hole ◽  
Black Hole Binaries ◽  
The Impact

scholarly journals Stellar hardening of massive black hole binaries: the impact of the host rotation

2021 ◽  
Vol 508 (1) ◽  
pp. 1533-1542
Author(s):  
Ludovica Varisco ◽  
Elisa Bortolas ◽  
Massimo Dotti ◽  
Alberto Sesana
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Equal Mass ◽  
Stellar Systems ◽  
Massive Black Hole ◽  
Loss Cone ◽  
Black Hole Binaries ◽  
Influence Radius ◽  
Three Body ◽  
The Impact

ABSTRACT Massive black hole binaries (MBHBs) with masses of ∼104 to $\sim 10^{10} \, \mathrm{M}_{\odot {}}$ are one of the main targets for currently operating and forthcoming space-borne gravitational wave observatories. In this paper, we explore the effect of the stellar host rotation on the bound binary hardening efficiency, driven by three-body stellar interactions. As seen in previous studies, we find that the centre of mass (CoM) of a prograde MBHB embedded in a rotating environment starts moving on a nearly circular orbit about the centre of the system shortly after the MBHB binding. In our runs, the oscillation radius is ≈ 0.25 (≈ 0.1) times the binary influence radius for equal mass MBHBs (MBHBs with mass ratio 1:4). Conversely, retrograde binaries remain anchored about the centre of the host. The binary shrinking rate is twice as fast when the binary CoM exhibits a net orbital motion, owing to a more efficient loss cone repopulation even in our spherical stellar systems. We develop a model that captures the CoM oscillations of prograde binaries; we argue that the CoM angular momentum gain per time unit scales with the internal binary angular momentum, so that most of the displacement is induced by stellar interactions occurring around the time of MBHB binding, while the subsequent angular momentum enhancement gets eventually quashed by the effect of dynamical friction. The effect of the background rotation on the MBHB evolution may be relevant for LISA sources, that are expected to form in significantly rotating stellar systems.

scholarly journals The TianQin project: Current progress on science and technology

2020 ◽  
Author(s):  
Jianwei Mei ◽  
Yan-Zheng Bai ◽  
Jiahui Bao ◽  
Enrico Barausse ◽  
Lin Cai ◽  
...  
Keyword(s):  
Black Hole ◽  
Ecliptic Plane ◽  
Mass Ratio ◽  
Massive Black Hole ◽  
Black Hole Binaries ◽  
Compact Binaries ◽  
Single Body ◽  
Science Operations ◽  
New Generation ◽  
Research Facilities

Abstract TianQin is a planned space-based gravitational wave (GW) observatory consisting of three Earth-orbiting satellites with an orbital radius of about $10^5 \, {\rm km}$. The satellites will form an equilateral triangle constellation the plane of which is nearly perpendicular to the ecliptic plane. TianQin aims to detect GWs between $10^{-4} \, {\rm Hz}$ and $1 \, {\rm Hz}$ that can be generated by a wide variety of important astrophysical and cosmological sources, including the inspiral of Galactic ultra-compact binaries, the inspiral of stellar-mass black hole binaries, extreme mass ratio inspirals, the merger of massive black hole binaries, and possibly the energetic processes in the very early universe and exotic sources such as cosmic strings. In order to start science operations around 2035, a roadmap called the 0123 plan is being used to bring the key technologies of TianQin to maturity, supported by the construction of a series of research facilities on the ground. Two major projects of the 0123 plan are being carried out. In this process, the team has created a new-generation $17 \, {\rm cm}$ single-body hollow corner-cube retro-reflector which was launched with the QueQiao satellite on 21 May 2018; a new laser-ranging station equipped with a $1.2 \, {\rm m}$ telescope has been constructed and the station has successfully ranged to all five retro-reflectors on the Moon; and the TianQin-1 experimental satellite was launched on 20 December 2019—the first-round result shows that the satellite has exceeded all of its mission requirements.

scholarly journals Accretion of clumpy cold gas onto massive black hole binaries: a possible fast route to binary coalescence

2018 ◽  
Vol 479 (3) ◽  
pp. 3438-3455 ◽  
Author(s):  
Felipe G Goicovic ◽  
Cristián Maureira-Fredes ◽  
Alberto Sesana ◽  
Pau Amaro-Seoane ◽  
Jorge Cuadra
Keyword(s):  
Black Hole ◽  
Massive Black Hole ◽  
Black Hole Binaries ◽  
Fast Route ◽  
Cold Gas

scholarly journals On the search of electromagnetic cosmological counterparts to coalescences of massive black hole binaries

2006 ◽  
Vol 372 (2) ◽  
pp. 869-875 ◽  
Author(s):  
M. Dotti ◽  
R. Salvaterra ◽  
A. Sesana ◽  
M. Colpi ◽  
F. Haardt
Keyword(s):  
Black Hole ◽  
Massive Black Hole ◽  
Black Hole Binaries

scholarly journals Massive Black Hole Binaries: Dynamical Evolution and Observational Signatures

2012 ◽  
Vol 2012 ◽  
pp. 1-14 ◽  
Author(s):  
M. Dotti ◽  
A. Sesana ◽  
R. Decarli
Keyword(s):  
Black Hole ◽  
Galaxy Formation ◽  
Dynamical Evolution ◽  
Wave Spectra ◽  
Galaxy Mergers ◽  
Massive Black Hole ◽  
Theoretical Understanding ◽  
Black Hole Binaries ◽  
Recent Developments ◽  
Open Issues

The study of the dynamical evolution of massive black hole pairs in mergers is crucial in the context of a hierarchical galaxy formation scenario. The timescales for the formation and the coalescence of black hole binaries are still poorly constrained, resulting in large uncertainties in the expected rate of massive black hole binaries detectable in the electromagnetic and gravitational wave spectra. Here, we review the current theoretical understanding of the black hole pairing in galaxy mergers, with a particular attention to recent developments and open issues. We conclude with a review of the expected observational signatures of massive binaries and of the candidates discussed in literature to date.

Sign in / Sign up

Export Citation Format

Share Document