scholarly journals Estimation of mass outflow rates from dissipative accretion disc around rotating black holes

2017 ◽  
Vol 471 (4) ◽  
pp. 4806-4819 ◽  
Author(s):  
Ramiz Aktar ◽  
Santabrata Das ◽  
Anuj Nandi ◽  
H. Sreehari
Keyword(s):  
Black Holes ◽  
Accretion Disc ◽  
Rotating Black Holes ◽  
Mass Outflow

scholarly journals Simulations of radiation driven winds from Keplerian discs

2020 ◽  
Author(s):  
Sananda Raychaudhuri ◽  
Mukesh K Vyas ◽  
Indranil Chattopadhyay
Keyword(s):  
Black Holes ◽  
Angular Momentum ◽  
Accretion Rate ◽  
Accretion Disc ◽  
Accretion Discs ◽  
Thermal Pressure ◽  
Linear Effect ◽  
Outflow Rate ◽  
Mass Outflow ◽  
Order Of Magnitude

Abstract We study the ejection of winds from thin accretion discs around stellar mass black holes and the time evolution of these winds in presence of radiation field generated by the accretion disc. Winds are produced by radiation, thermal pressure and the centrifugal force of the disc. The winds are found to be mildly relativistic, with speeds reaching up to terminal speeds 0.1 for accretion rate 4 in Eddington units. We show that the ejected matter gets its rotation by transporting angular momentum from the disc to the wind. We also show that the radiation drag affects the accretion disc winds in a very significant manner. Not only that the terminal speeds are reduced by an order of magnitude due to radiation drag, but we also show that the non-linear effect of radiation drag, can mitigate the formation of the winds from the matter ejected by the accretion disc. As radiation drag reduces the velocity of the wind, the mass outflow rate is reduced in its presence as well.

scholarly journals Simulation of AGN feedback and its impact on galaxies

2016 ◽  
Vol 12 (S324) ◽  
pp. 231-234
Author(s):  
Martin A. Bourne
Keyword(s):  
Black Holes ◽  
Large Scale ◽  
Accretion Disc ◽  
Moving Mesh ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Mass Outflow ◽  
Phase Medium ◽  
Energy Conserving ◽  
Multi Phase

AbstractFeedback released during the growth of supermassive black holes is expected to play a key role in shaping black hole-host galaxy co-evolution. Powerful, accretion disc driven winds have been invoked to explain both observed scaling relations (e.g., M − σ) and large-scale outflows with mass outflow rates of ~ 100 − 1000 M⊙ yr−1 and momentum rates of up to ~ 30 LAGN/c. Critically, how these winds couple to the host galaxy depends on if they are momentum or energy conserving. I outline observational signatures that could distinguish between these regimes and discuss their roles in establishing galaxy properties. Furthermore, I discuss high-resolution simulations exploring feedback in a multi-phase medium, highlighting how structural properties of galaxies can impact feedback efficiency. Finally, feedback, in the form of collimated jets, is expected to regulate cooling in galaxy clusters. I discuss new simulations of jet feedback using the moving-mesh code AREPO and outline the scope of our new study.

scholarly journals Mass-loss from advective accretion disc around rotating black holes

2015 ◽  
Vol 453 (4) ◽  
pp. 3415-3428 ◽  
Author(s):  
Ramiz Aktar ◽  
Santabrata Das ◽  
Anuj Nandi
Keyword(s):  
Black Holes ◽  
Mass Loss ◽  
Accretion Disc ◽  
Rotating Black Holes

scholarly journals A maximum X-ray luminosity scale of disc-dominated tidal destruction events

2021 ◽  
Author(s):  
Andrew Mummery
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Compton Scattering ◽  
Large Mass ◽  
Accretion Disc ◽  
Black Hole Mass ◽  
X Ray ◽  
Soft State ◽  
Mass Outflow ◽  
Strong Agreement

Abstract We develop a model describing the dynamical and observed properties of disc-dominated TDEs around black holes with the lowest masses (M ≲ few × 106M⊙). TDEs around black holes with the lowest masses are most likely to reach super-Eddington luminosities at early times in their evolution. By assuming that the amount of stellar debris which can form into a compact accretion disc is set dynamically by the Eddington luminosity, we make a number of interesting and testable predictions about the observed properties of bright soft-state X-ray TDEs and optically bright, X-ray dim TDEs. We argue that TDEs around black holes of the lowest masses will expel the vast majority of their gravitationally bound debris into a radiatively driven outflow. A large-mass outflow will obscure the innermost X-ray producing regions, leading to a population of low black hole mass TDEs which are only observed at optical & UV energies. TDE discs evolving with bolometric luminosities comparable to their Eddington luminosity will have near constant (i.e. black hole mass independent) X-ray luminosities, of order LX, max ≡ LM ∼ 1043 − 1044 erg/s. The range of luminosity values stems primarily from the range of allowed black hole spins. A similar X-ray luminosity limit exists for X-ray TDEs in the hard (Compton scattering dominated) state, and we therefore predict that the X-ray luminosity of the brightest X-ray TDEs will be at the scale LM(a) ∼ 1043 − 1044 erg/s, independent of black hole mass and accretion state. These predictions are in strong agreement with the properties of the existing population (∼40 sources) of observed TDEs.

scholarly journals Black hole hair removal for N = 4 CHL models

2021 ◽  
Vol 2021 (2) ◽  
Author(s):  
Subhroneel Chakrabarti ◽  
Suresh Govindarajan ◽  
P. Shanmugapriya ◽  
Yogesh K. Srivastava ◽  
Amitabh Virmani
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Degrees Of Freedom ◽  
Microscopic Analysis ◽  
Flat Space ◽  
Special Care ◽  
Hair Removal ◽  
Partition Functions ◽  
Rotating Black Holes

Abstract Although BMPV black holes in flat space and in Taub-NUT space have identical near-horizon geometries, they have different indices from the microscopic analysis. For K3 compactification of type IIB theory, Sen et al. in a series of papers identified that the key to resolving this puzzle is the black hole hair modes: smooth, normalisable, bosonic and fermionic degrees of freedom living outside the horizon. In this paper, we extend their study to N = 4 CHL orbifold models. For these models, the puzzle is more challenging due to the presence of the twisted sectors. We identify hair modes in the untwisted as well as twisted sectors. We show that after removing the contributions of the hair modes from the microscopic partition functions, the 4d and 5d horizon partition functions agree. Special care is taken to present details on the smoothness analysis of hair modes for rotating black holes, thereby filling an essential gap in the literature.

scholarly journals Rotating black holes in massive gravity

2014 ◽  
Vol 90 (8) ◽  
Author(s):  
Eugeny Babichev ◽  
Alessandro Fabbri
Keyword(s):  
Black Holes ◽  
Massive Gravity ◽  
Rotating Black Holes

scholarly journals Superradiance Resonance Cavity Outside Rapidly Rotating Black Holes

2000 ◽  
Vol 84 (20) ◽  
pp. 4537-4540 ◽  
Author(s):  
Nils Andersson ◽  
Kostas Glampedakis
Keyword(s):  
Black Holes ◽  
Rotating Black Holes ◽  
Resonance Cavity
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