Start Date
10-17-2017 10:00 AM
Description
Observations of high-redshift quasars reveal that super massive black holes (SMBHs) with masses exceeding 109 M⊙ formed as early as redshift z ~ 7 [1,3,6]. This means that SMBHs have already formed ~700 million years after the Big Bang. How did such SMBHs could grow so quickly?
In this work, we use a modified and improved version of the blockstructured adaptive mesh refinement (AMR) code ENZO [2] to provide high spatial and temporal resolution for modeling the formation of SMBHs via direct collapse within dark matter (DM) halos at high redshifts. The radiation hydrodynamics equations are solved in the flux-limited diffusion (FLD) approximation in the full cosmological background [5]. The chemical species are assumed to be in local thermodynamic equilibrium (LTE). We follow the evolution of the collapsing gas from a kilo-parsec scale down to 0.001 AU --- 11 decades in radius.
Formation of Supermassive Black Holes in the Early Universe: High-Resolution Numerical Simulations of Radiation Transfer Inside Collapsing Gas
Observations of high-redshift quasars reveal that super massive black holes (SMBHs) with masses exceeding 109 M⊙ formed as early as redshift z ~ 7 [1,3,6]. This means that SMBHs have already formed ~700 million years after the Big Bang. How did such SMBHs could grow so quickly?
In this work, we use a modified and improved version of the blockstructured adaptive mesh refinement (AMR) code ENZO [2] to provide high spatial and temporal resolution for modeling the formation of SMBHs via direct collapse within dark matter (DM) halos at high redshifts. The radiation hydrodynamics equations are solved in the flux-limited diffusion (FLD) approximation in the full cosmological background [5]. The chemical species are assumed to be in local thermodynamic equilibrium (LTE). We follow the evolution of the collapsing gas from a kilo-parsec scale down to 0.001 AU --- 11 decades in radius.
