scholarly journals Long‐Term Evolution of Massive Black Hole Binaries. III. Binary Evolution in Collisional Nuclei

2007 ◽  
Vol 671 (1) ◽  
pp. 53-72 ◽  
Author(s):  
David Merritt ◽  
Seppo Mikkola ◽  
Andras Szell
Keyword(s):  
Black Hole ◽  
Long Term Evolution ◽  
Massive Black Hole ◽  
Black Hole Binaries ◽  
Term Evolution ◽  
Binary Evolution

Long‐Term Evolution of Massive Black Hole Binaries

2003 ◽  
Vol 596 (2) ◽  
pp. 860-878 ◽  
Author(s):  
Miloš Milosavljević ◽  
David Merritt
Keyword(s):  
Black Hole ◽  
Long Term Evolution ◽  
Massive Black Hole ◽  
Black Hole Binaries ◽  
Term Evolution

A new method to simulate long-term evolution of stars near a massive Black Hole

2019 ◽  
Vol 14 (S351) ◽  
pp. 434-437
Author(s):  
Y. Funato
Keyword(s):  
Black Hole ◽  
Galactic Center ◽  
Time Integration ◽  
Star Clusters ◽  
Long Term Evolution ◽  
Massive Black Hole ◽  
Simple Method ◽  
Time Integration Method ◽  
Term Evolution

AbstractN-body simulation is the necessary tool to investigate the evolution of star clusters. It is important to develop a time integration method which guarantees the appropriate accuracy and calculation cost.Here we present a new simple method for long term simulation of stars around a massive black hole in stellar systems. Usually the time integration orbits of stars revolving a massive black hole requires much simulation time. We introduce a time transformation which is a kind of ”inverse KS regularization” of time. Using our method, the integration of the long term evolution near a black hole (BH) becomes easier, especially applied to relatively large star clusters and the Galactic Center.

scholarly journals Supermassive black hole seed formation at high redshifts: long-term evolution of the direct collapse

2015 ◽  
Vol 456 (1) ◽  
pp. 500-511 ◽  
Author(s):  
Isaac Shlosman ◽  
Jun-Hwan Choi ◽  
Mitchell C. Begelman ◽  
Kentaro Nagamine
Keyword(s):  
Black Hole ◽  
Long Term Evolution ◽  
Seed Formation ◽  
Supermassive Black Hole ◽  
Term Evolution

scholarly journals Formation of counter-rotating and highly eccentric massive black hole binaries in galaxy mergers

2021 ◽  
Vol 503 (1) ◽  
pp. 498-510
Author(s):  
Imran Tariq Nasim ◽  
Cristobal Petrovich ◽  
Adam Nasim ◽  
Fani Dosopoulou ◽  
Fabio Antonini
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Dynamical Evolution ◽  
Orbital Plane ◽  
Equal Mass ◽  
Galaxy Mergers ◽  
High Eccentricity ◽  
Massive Black Hole ◽  
Black Hole Binaries ◽  
Binary Evolution

ABSTRACT Supermassive black hole (SMBH) binaries represent the main target for missions such as the Laser Interferometer Space Antenna and Pulsar Timing Arrays. The understanding of their dynamical evolution prior to coalescence is therefore crucial to improving detection strategies and for the astrophysical interpretation of the gravitational wave data. In this paper, we use high-resolution N-body simulations to model the merger of two equal-mass galaxies hosting a central SMBH. In our models, all binaries are initially prograde with respect to the galaxy sense of rotation. But, binaries that form with a high eccentricity, e ≳ 0.7, quickly reverse their sense of rotation and become almost perfectly retrograde at the moment of binary formation. The evolution of these binaries proceeds towards larger eccentricities, as expected for a binary hardening in a counter-rotating stellar distribution. Binaries that form with lower eccentricities remain prograde and at comparatively low eccentricities. We study the origin of the orbital flip by using an analytical model that describes the early stages of binary evolution. This model indicates that the orbital plane flip is due to the torque from the triaxial background mass distribution that naturally arises from the galactic merger process. Our results imply the existence of a population of SMBH binaries with a high eccentricity and could have significant implications for the detection of the gravitational wave signal emitted by these systems.

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