scholarly journals The Pairing of Accreting Massive Black Holes in Multiphase Circumnuclear Disks: the Interplay Between Radiative Cooling, Star Formation, and Feedback Processes

2017 ◽  
Vol 838 (1) ◽  
pp. 13 ◽  
Author(s):  
Rafael Souza Lima ◽  
Lucio Mayer ◽  
Pedro R. Capelo ◽  
Jillian M. Bellovary
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Radiative Cooling ◽  
Massive Black Holes

scholarly journals JD8 - Hot Interstellar Matter in Elliptical Galaxies

2009 ◽  
Vol 5 (H15) ◽  
pp. 269-270
Author(s):  
Dong-Woo Kim ◽  
Silvia Pellegrini
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Analytical Modeling ◽  
Elliptical Galaxies ◽  
Theoretical Studies ◽  
Interstellar Matter ◽  
Significant Progress ◽  
Massive Black Holes ◽  
X Ray ◽  
Formation And Evolution

The physical properties of the hot interstellar matter in elliptical galaxies are directly related with the formation and evolution of elliptical galaxies via star formation episodes, environmental effects such as stripping, infall, and mergers, and growth of super-massive black holes. The recent successful Chandra and XMM-Newton X-ray space missions have provided a large amount of high spatial/spectral resolution observational data on the hot ISM in elliptical galaxies. At the same time, theoretical studies with numerical simulations and analytical modeling of the dynamical and chemical evolution of elliptical galaxies have made a significant progress and start to predict various observable quantities.

scholarly journals Star formation in accretion discs and SMBH growth

2020 ◽  
Vol 493 (3) ◽  
pp. 3732-3743 ◽  
Author(s):  
Alexander J Dittmann ◽  
M Coleman Miller
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Active Galactic Nuclei ◽  
Accretion Rate ◽  
High Redshift ◽  
Galactic Nuclei ◽  
Compact Objects ◽  
Accretion Discs ◽  
Massive Black Holes ◽  
Gas Accretion

ABSTRACT Accretion discs around active galactic nuclei (AGNs) are potentially unstable to star formation at large radii. We note that when the compact objects formed from some of these stars spiral into the central supermassive black hole (SMBH), there is no radiative feedback and therefore the accretion rate is not limited by radiation forces. Using a set of accretion disc models, we calculate the accretion rate on to the central SMBH in both gas and compact objects. We find that the time-scale for an SMBH to double in mass can decrease by factors ranging from ∼0.7 to as low as ∼0.1 in extreme cases, compared to gas accretion alone. Our results suggest that the formation of extremely massive black holes at high redshift may occur without prolonged super-Eddington gas accretion or very massive seed black holes. We comment on potential observational signatures as well as implications for other observations of AGNs.

scholarly journals Feedback from central massive black holes in galaxies using cosmological simulations

2019 ◽  
Vol 15 (S359) ◽  
pp. 35-36
Author(s):  
Paramita Barai
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Galaxy Evolution ◽  
Supermassive Black Holes ◽  
Active Galaxies ◽  
Host Galaxies ◽  
Massive Black Holes ◽  
Energy Feedback ◽  
Hydrodynamical Simulations ◽  
Gas Accretion

AbstractGas accretion onto central supermassive black holes of active galaxies and resulting energy feedback, is an important component of galaxy evolution, whose details are still unknown especially at early cosmic epochs. We investigate BH growth and feedback in quasar-host galaxies at z ⩾ 6 by performing cosmological hydrodynamical simulations. We simulate the 2R200 region around a 2 × 1012Mʘ halo at z = 6, inside a (500 Mpc)3 comoving volume, using the zoom-in technique. We find that BHs accrete gas at the Eddington rate over z = 9–6. At z = 6, our most-massive BH has grown to MBH = 4 × 109 Mʘ. Star-formation is quenched over z = 8–6.

Conference Summary

2017 ◽  
Vol 13 (S336) ◽  
pp. 451-454
Author(s):  
Philip J. Diamond
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Interstellar Medium ◽  
Massive Black Holes ◽  
Conference Summary ◽  
Evolved Stars ◽  
The Universe

AbstractIAU Symposium 336, Astrophysical Masers: Unlocking the Mysteries of the Universe, took place between 4 - 8 September, 2017 in Cagliari, on the beautiful island of Sardinia. The Symposium, the fifth focusing on masers as a tool for astrophysics, was dedicated to our friend and colleague Malcolm Walmsley, who sadly passed away shortly before the meeting. To quote Karl Menten: “Malcolm made numerous fundamental contributions to our understanding of the physics and chemistry of star formation and the interstellar medium. He was an exceptional scientist, a highly esteemed colleague and a true gentleman”. Vale Malcolm. The topics discussed at the symposium covered a huge range, from star-formation, evolved stars, galaxies and their constituents, super-massive black-holes to cosmology.

scholarly journals Equal and Unequal-Mass Mergers of Disk and Elliptical Galaxies with Black Holes

2009 ◽  
Vol 5 (S267) ◽  
pp. 461-461
Author(s):  
Peter H. Johansson ◽  
Thorsten Naab ◽  
Andreas Burkert
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Accretion Rate ◽  
Rest Mass ◽  
Elliptical Galaxies ◽  
Radiative Cooling ◽  
Early Type ◽  
Mass Energy ◽  
Binary Galaxy ◽  
Supernova Feedback

We present binary galaxy merger simulations of gas-rich disks (Sp-Sp), of early-type galaxies and disks (E-Sp, mixed mergers), and mergers of early-type galaxies (E-E, dry mergers) including radiative cooling, star formation, black hole (BH) accretion, and the associated feedback processes. The numerical simulations include cooling, star formation, supernova feedback, and BH accretion modeled following a Bondi–Hoyle accretion parameterization. The maximum accretion rate is limited to the Eddington rate, with a total of 0.5% of the accreted rest-mass energy distributed as thermal energy to the surrounding gas.

scholarly journals Fueling-controlled growth of massive black holes

2007 ◽  
Vol 3 (S245) ◽  
pp. 165-168
Author(s):  
Andrés Escala
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Numerical Simulations ◽  
Accretion Disk ◽  
Gravitational Potential ◽  
Controlled Growth ◽  
Massive Black Holes ◽  
Depletion Rate

AbstractWe study the relation between nuclear massive black holes and their host spheroid gravitational potential. Using AMR numerical simulations, we analyze how gas is transported into the nuclear (central kpc) regions of galaxies. We study gas fueling onto the inner accretion disk (sub-pc scale) and star formation in a massive nuclear disk like those generally found in proto-spheroids (ULIRGs, SCUBA Galaxies). These sub-pc resolution simulations of gas fueling, which is mainly depleted by star formation, naturally satisfy the ‘MBH- Mvirial’ relation, with a scatter considerably less than that observed. We find that a generalized version of the Kennicutt-Schmidt Law for starbursts is satisfied, in which the total gas depletion rate (Ṁgas= ṀBH+ ṀSF) scales as Mgas/torbital.

scholarly journals The evolution of high-redshift massive black holes

2015 ◽  
Vol 11 (S319) ◽  
pp. 72-79 ◽  
Author(s):  
Marta Volonteri ◽  
Melanie Habouzit ◽  
Fabio Pacucci ◽  
Michael Tremmel
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Galaxy Evolution ◽  
Milky Way ◽  
High Redshift ◽  
Theoretical Models ◽  
Host Galaxies ◽  
Massive Black Holes ◽  
Rate Feedback ◽  
First Galaxies

AbstractMassive black holes (MBHs) are nowadays recognized as integral parts of galaxy evolution. Both the approximate proportionality between MBH and galaxy mass, and the expected importance of feedback from active MBHs in regulating star formation in their host galaxies point to a strong interplay between MBHs and galaxies. MBHs must form in the first galaxies and be fed by gas in these galaxies, with continuous or intermittent inflows that, at times, can be larger than the Eddington rate. Feedback from supernovae and from the MBHs themselves modulates the growth of the first MBHs. While current observational data only probe the most massive and luminous MBHs, the tip of the iceberg, we will soon be able to test theoretical models of MBH evolution on more “normal” MBHs: the MBHs that are indeed relevant in building the population that we observe in local galaxies, including our own Milky Way.

Sign in / Sign up

Export Citation Format

Share Document