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Full-Text Articles in Physical Sciences and Mathematics
Formation Of Supermassive Black Holes In The Early Universe: High-Resolution Numerical Simulations Of Radiation Transfer Inside Collapsing Gas, Yang Luo, Kazem Ardaneh, Isaac Shlosman, Kentaro Nagamine, John Wise, Mitchell C. Begelman
Formation Of Supermassive Black Holes In The Early Universe: High-Resolution Numerical Simulations Of Radiation Transfer Inside Collapsing Gas, Yang Luo, Kazem Ardaneh, Isaac Shlosman, Kentaro Nagamine, John Wise, Mitchell C. Begelman
Commonwealth Computational Summit
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 …
Evolution Of Barred Galaxies In Spinning Dark Matter Halos: High Resolution N-Body Simulations At Dlx, Angela Collier, Isaac Shlosman, Clayton Heller
Evolution Of Barred Galaxies In Spinning Dark Matter Halos: High Resolution N-Body Simulations At Dlx, Angela Collier, Isaac Shlosman, Clayton Heller
Commonwealth Computational Summit
Observations show that galaxies are dominated by stellar disks immersed in much more massive, slowly tumbling dark matter (DM) halos. Large fraction of galactic disks, at least 75%, are barred (see Hubble Fork on the right). Stellar bars form either via spontaneous break of axial symmetry or via galaxy interactions.
The formation and evolution of stellar bars is not fully understood. Stellar bar evolution is highly nonlinear and cannot be treated analytically. The main approach to study these disk-halo systems is via numerical simulations, whose goal is to explain why galaxies have such a wide range of morphologies as shown …