scholarly journals Equation of State and Progenitor Dependence of Stellar-mass Black Hole Formation

2020 ◽  
Vol 894 (1) ◽  
pp. 4 ◽  
Author(s):  
André da Silva Schneider ◽  
Evan O’Connor ◽  
Elvira Granqvist ◽  
Aurore Betranhandy ◽  
Sean M. Couch
Keyword(s):  
Black Hole ◽  
Equation Of State ◽  
Stellar Mass ◽  
Hole Formation ◽  
Black Hole Formation

scholarly journals Equation of State Dependent Dynamics and Multi-messenger Signals from Stellar-mass Black Hole Formation

2018 ◽  
Vol 857 (1) ◽  
pp. 13 ◽  
Author(s):  
Kuo-Chuan Pan ◽  
Matthias Liebendörfer ◽  
Sean M. Couch ◽  
Friedrich-Karl Thielemann
Keyword(s):  
Black Hole ◽  
Equation Of State ◽  
Stellar Mass ◽  
Hole Formation ◽  
Black Hole Formation ◽  
State Dependent

Gravitational collapse of dust fluid and dark energy in the presence of curvature: Black hole formation

2019 ◽  
Vol 34 (29) ◽  
pp. 1950240 ◽  
Author(s):  
Syed Zaheer Abbas ◽  
Hasrat Hussain Shah ◽  
Huafei Sun ◽  
Farook Rahaman ◽  
Faizuddin Ahmed
Keyword(s):  
Black Hole ◽  
Dark Energy ◽  
Equation Of State ◽  
Gravitational Collapse ◽  
Dust Cloud ◽  
Curvature Effect ◽  
Hole Formation ◽  
Black Hole Formation ◽  
State Formula ◽  
Dust Fluid

Study of gravitational collapse and black hole formation has got much interest in recent years after gravitational waves detection from mergers of black hole binaries. Here, we studied the gravitational collapse of a spherically symmetric clump of matter, constituted of dust fluid, [Formula: see text], in a background of dark energy, [Formula: see text]. We investigate the curvature effect [Formula: see text] on the gravitational collapsing process. Gravitational collapsing process for two different cases is discussed i.e. collapse of dust cloud only and collapse of dark energy. We used equation of state [Formula: see text], [Formula: see text]. For dark energy case, we discuss the collapsing process and curvature effect for different parameter values of equation of state.

scholarly journals NIHAO – XXII. Introducing black hole formation, accretion, and feedback into the NIHAO simulation suite

2019 ◽  
Vol 487 (4) ◽  
pp. 5476-5489 ◽  
Author(s):  
Marvin Blank ◽  
Andrea V Macciò ◽  
Aaron A Dutton ◽  
Aura Obreja
Keyword(s):  
Black Hole ◽  
Black Hole Physics ◽  
Elliptical Galaxies ◽  
Stellar Mass ◽  
High Mass ◽  
Mass Relation ◽  
Hole Formation ◽  
Black Hole Formation ◽  
Astrophysical Objects ◽  
Halo Masses

ABSTRACT We introduce algorithms for black hole physics, i.e. black hole formation, accretion, and feedback, into the Numerical Investigation of a Hundred Astrophysical Objects (NIHAO) project of galaxy simulations. This enables us to study high mass, elliptical galaxies, where feedback from the central black hole is generally thought to have a significant effect on their evolution. We furthermore extend the NIHAO suite by 45 simulations that encompass z = 0 halo masses from 1 × 1012 to $4 \times 10^{13}\, \mathrm{M}_{\odot }$, and resimulate five galaxies from the original NIHAO sample with black hole physics, which have z = 0 halo masses from 8 × 1011 to $3 \times 10^{12}\, \mathrm{M}_{\odot }$. Now NIHAO contains 144 different galaxies and thus has the largest sample of zoom-in simulations of galaxies, spanning z = 0 halo masses from 9 × 108 to $4 \times 10^{13}\, \mathrm{M}_{\odot }$. In this paper we focus on testing the algorithms and calibrating their free parameters against the stellar mass versus halo mass relation and the black hole mass versus stellar mass relation. We also investigate the scatter of these relations, which we find is a decreasing function with time and thus in agreement with observations. For our fiducial choice of parameters we successfully quench star formation in objects above a z = 0 halo mass of $10^{12}\, \mathrm{M}_{\odot }$, thus transforming them into red and dead galaxies.

scholarly journals Bekenstein–Hawking entropy in expanding universes from black hole theorems

2014 ◽  
Vol 29 (17) ◽  
pp. 1450091 ◽  
Author(s):  
Stefano Viaggiu
Keyword(s):  
Black Hole ◽  
Equation Of State ◽  
Ideal Gas ◽  
Hole Formation ◽  
Black Hole Evaporation ◽  
Black Hole Formation ◽  
Hubble Radius ◽  
Primordial Inflation ◽  
The One

We show that the use of suitable theorems for black hole formation in Friedmann expanding universes leads to a modification of the Bekenstein–Hawking entropy. By adopting an argument similar to the original Bekenstein one, we write down the expression for the Bekenstein–Hawking entropy suitable for non-static isotropic expanding universes together with the equation of state of a black hole. This equation can be put in a form similar to the one of an ideal gas but with a factor depending on the Hubble radius. Moreover, we give some argument on a possible relation between our entropy expression and the Cardy–Verlinde one. Finally, we explore the possibility that primordial inflation is due to black hole evaporation in our context.

scholarly journals Feeding and feedback from little monsters: AGN in dwarf galaxies

2020 ◽  
Vol 15 (S359) ◽  
pp. 238-242
Author(s):  
Mar Mezcua
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Early Universe ◽  
Dwarf Galaxies ◽  
Scaling Relations ◽  
Strong Impact ◽  
Hole Formation ◽  
Intermediate Mass ◽  
Black Hole Formation ◽  
Low Mass

AbstractDetecting the seed black holes from which quasars formed is extremely challenging; however, those seeds that did not grow into supermassive should be found as intermediate-mass black holes (IMBHs) of 100 – 105 M⊙ in local dwarf galaxies. The use of deep multiwavelength surveys has revealed that a population of actively accreting IMBHs (low-mass AGN) exists in dwarf galaxies at least out to z ˜3. The black hole occupation fraction of these galaxies suggests that the early Universe seed black holes formed from direct collapse of gas, which is reinforced by the possible flattening of the black hole-galaxy scaling relations at the low-mass end. This scenario is however challenged by the finding that AGN feedback can have a strong impact on dwarf galaxies, which implies that low-mass AGN in dwarf galaxies might not be the untouched relics of the early seed black holes. This has important implications for seed black hole formation models.

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