GALAXY FORMATION WITH SELF-CONSISTENTLY MODELED STARS AND MASSIVE BLACK HOLES. I. FEEDBACK-REGULATED STAR FORMATION AND BLACK HOLE GROWTH

@article{Kim2011GALAXYFW,
  title={GALAXY FORMATION WITH SELF-CONSISTENTLY MODELED STARS AND MASSIVE BLACK HOLES. I. FEEDBACK-REGULATED STAR FORMATION AND BLACK HOLE GROWTH},
  author={Ji-hoon Kim and John H. Wise and Marcelo A. Alvarez and Tom Abel},
  journal={The Astrophysical Journal},
  year={2011},
  volume={738}
}
There is mounting evidence for the coevolution of galaxies and their embedded massive black holes (MBHs) in a hierarchical structure formation paradigm. To tackle the nonlinear processes of galaxy—MBH interaction, we describe a self-consistent numerical framework which incorporates both galaxies and MBHs. The high-resolution adaptive mesh refinement (AMR) code Enzo is modified to model the formation and feedback of molecular clouds at their characteristic scale of 15.2 pc and the accretion of… 
Gas inflow and star formation near supermassive black holes: the role of nuclear activity
Numerical models of gas inflow towards a supermassive black hole (SMBH) show that star formation may occur in such an environment through the growth of a gravitationally unstable gas disc. We
On the dynamics of supermassive black holes in gas-rich, star-forming galaxies: the case for nuclear star cluster co-evolution
We introduce a new model for the formation and evolution of supermassive black holes (SMBHs) in the RAMSES code using sink particles, improving over previous work the treatment of gas accretion and
Radiation-driven Turbulent Accretion onto Massive Black Holes
Accretion of gas and interaction of matter and radiation are at the heart of many questions pertaining to black hole (BH) growth and coevolution of massive BHs and their host galaxies. To answer
A model for cosmological simulations of galaxy formation physics: multi-epoch validation
We present a multi-epoch analysis of the galaxy populations formed within the cosmological hydrodynamical simulations presented in Vogelsberger et al. (2013). These simulations explore the
Cosmological direct-collapse black hole formation sites hostile for their growth
The direct collapse (DC) is a promising mechanism that provides massive seed black holes (BHs) with ∼105 M⊙ in the early universe. To study a long-term accretion growth of a direct-collapse black
DWARF GALAXIES WITH IONIZING RADIATION FEEDBACK. II. SPATIALLY RESOLVED STAR FORMATION RELATION
We investigate the spatially resolved star formation relation using a galactic disk formed in a comprehensive high-resolution (3.8 pc) simulation. Our new implementation of stellar feedback includes
BLACK HOLE–GALAXY CORRELATIONS WITHOUT SELF-REGULATION
Recent models of black hole growth in a cosmological context have forwarded a paradigm in which the growth is self-regulated by feedback from the black hole itself. Here we use cosmological zoom
Can AGN feedback-driven star formation explain the size evolution of massive galaxies?
Observations indicate that massive galaxies at z~2 are more compact than galaxies of comparable mass at z~0, with effective radii evolving by a factor of ~3-5. This implies that galaxies grow
DWARF GALAXIES WITH IONIZING RADIATION FEEDBACK. I. ESCAPE OF IONIZING PHOTONS
We describe a new method for simulating ionizing radiation and supernova feedback in the analogs of low-redshift galactic disks. In this method, which we call star-forming molecular cloud (SFMC)
Comparison of black hole growth in galaxy mergers with gasoline and ramses
Supermassive black hole dynamics during galaxy mergers is crucial in determining the rate of black hole mergers and cosmic black hole growth. As simulations achieve higher resolution, it becomes
...
...

References

SHOWING 1-10 OF 145 REFERENCES
Mass distribution in galaxy clusters: the role of Active Galactic Nuclei feedback
We use 1-kpc resolution cosmological Adaptive Mesh Refinement (AMR) simulations of a Virgo-like galaxy cluster to investigate the effect of feedback from supermassive black holes on the mass
Cosmological simulations of the growth of supermassive black holes and feedback from active galactic nuclei: method and tests
We present a method that self-consistently tracks the growth of supermassive black holes (BHs) and the feedback from active galactic nuclei (AGN) in cosmological, hydrodynamical simulations. Our
How do massive black holes get their gas
We use multiscale smoothed particle hydrodynamic simulations to study the inflow of gas from galactic scales (∼10 kpc) down to ≲ 0.1 pc, at which point the gas begins to resemble a traditional,
Modelling feedback from stars and black holes in galaxy mergers
We describe techniques for incorporating feedback from star formation and black hole (BH) accretion into simulations of isolated and merging galaxies. At present, the details of these processes
Radiative feedback from quasars and the growth of massive black holes in stellar spheroids
We discuss the importance of feedback via photoionization and Compton heating on the co-evolution of massive black holes (MBHs) at the centre of spheroidal galaxies, and their stellar and gaseous
FEEDBACK FROM CENTRAL BLACK HOLES IN ELLIPTICAL GALAXIES. II. CAN PURELY MECHANICAL ENERGY FEEDBACK MODELS WORK?
By using high-resolution one-dimensional hydrodynamical simulations, we investigate the effects of purely mechanical feedback from super massive black holes (SMBHs) in the evolution of elliptical
Radiative Feedback from Massive Black Holes in Elliptical Galaxies: AGN Flaring and Central Starburst Fueled by Recycled Gas
We show how the observed AGN radiative output from massive black holes at the centers of elliptical galaxies affects the hot ISM of these systems with the aid of a high-resolution hydrodynamical
FEEDBACK FROM CENTRAL BLACK HOLES IN ELLIPTICAL GALAXIES. I. MODELS WITH EITHER RADIATIVE OR MECHANICAL FEEDBACK BUT NOT BOTH
The importance of the radiative feedback from massive black holes at the centers of elliptical galaxies is not in doubt, given the well-established relations among electromagnetic output, black hole
GROWING MASSIVE BLACK HOLE PAIRS IN MINOR MERGERS OF DISK GALAXIES
We perform a suite of high-resolution smoothed particle hydrodynamics simulations to investigate the orbital decay and mass evolution of massive black hole (MBH) pairs down to scales of ∼30 pc during
GALAXY MERGERS WITH ADAPTIVE MESH REFINEMENT: STAR FORMATION AND HOT GAS OUTFLOW
In hierarchical structure formation, merging of galaxies is frequent and known to dramatically affect their properties. To comprehend these interactions high-resolution simulations are indispensable
...
...