scholarly journals Non-steady-state long-term evolution of supermassive black hole binaries surrounded by accretion discs

2018 ◽  
Vol 482 (4) ◽  
pp. 4383-4396 ◽  
Author(s):  
Camilo Fontecilla ◽  
Zoltán Haiman ◽  
Jorge Cuadra
Keyword(s):  
Black Hole ◽  
Steady State ◽  
Long Term Evolution ◽  
Accretion Discs ◽  
Black Hole Binaries ◽  
Supermassive Black Hole ◽  
Term 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

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 Evolution of supermassive black hole binaries in gaseous environments

2015 ◽  
Vol 11 (A29B) ◽  
pp. 314-316
Author(s):  
Giuseppe Lodato
Keyword(s):  
Black Hole ◽  
Mass Flow ◽  
Dynamical Evolution ◽  
Equal Mass ◽  
Accretion Discs ◽  
Tidal Torque ◽  
Black Hole Binaries ◽  
Supermassive Black Hole ◽  
Binary Component ◽  
Flow Through

AbstractIn this contribution, I discuss some aspects of the dynamical evolution of supermassive black hole binaries and their accretion discs. Firstly, I discuss the issue of alignment of the spins of the two binary component, which has important implications for the shape of the gravitational wave emitted at merger and for the possibility of a strong recoil of the remnant black hole. Even under the favourable assumption that mass flow through the gap is not inhibited by tidal torque, we demonstrate that differential accretion onto the two components of the systems results in a very different spin evolution of the two black holes. Secondly, I revisit the issue of how much mass can flow within the cavity carved in the disc by an equal mass binary. Recent simulations have shown that the tidal torque of the binary is generally not sufficient to prevent accretion onto the binary component. Here, I demonstrate that such results are heavily dependent on the disc thickness. While for H/R ~ 0.1 (the value adopted in most simulations to date), we reproduce the previous results, we show that as H/R is decreased to ~ 0.01, mass flow through the gap is essentially shut off almost completely. Thirdly, I show numerical simulations of the process of gas squeezing during the merger proper, demonstrating that most of the disc mass is accreted producing a super-Eddington flare.

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