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Title: Numerical simulations of optically thick accretion onto a black hole. I. Spherical case

Abstract

Modeling the radiation generated by accreting matter is an important step toward realistic simulations of black hole accretion disks, especially at high accretion rates. To this end, we have recently added radiation transport to the existing general relativistic magnetohydrodynamic code, Cosmos++. However, before attempting to model radiative accretion disks, we have tested the new code using a series of shock tube and Bondi (spherical inflow) problems. The four radiative shock tube tests, first presented by Farris et al., have known analytic solutions, allowing us to calculate errors and convergence rates for our code. The Bondi problem only has an analytic solution when radiative processes are ignored, but it is pertinent because it is closer to the physics we ultimately want to study. In our simulations, we include Thomson scattering and thermal bremsstrahlung in the opacity, focusing exclusively on the super-Eddington regime. Unlike accretion onto bodies with solid surfaces, super-Eddington accretion onto black holes does not produce super-Eddington luminosity. In our examples, despite accreting at up to 300 times the Eddington rate, our measured luminosity is always several orders of magnitude below Eddington.

Authors:
 [1];  [1];  [1];  [1];  [2]
  1. College of Charleston, Charleston, SC (United States)
  2. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Publication Date:
Research Org.:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF); UT-Battelle LLC/ORNL, Oak Ridge, TN (Unted States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1564878
Grant/Contract Number:  
AC05-00OR22725
Resource Type:
Accepted Manuscript
Journal Name:
Astrophysical Journal, Supplement Series
Additional Journal Information:
Journal Volume: 201; Journal Issue: 2; Journal ID: ISSN 0067-0049
Publisher:
American Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics; accretion, accretion disks; black hole physics; magnetohydrodynamics (MHD); methods: numerical; radiative transfer

Citation Formats

Fragile, P. Chris, Gillespie, Anna, Monahan, Timothy, Rodriguez, Marco, and Anninos, Peter. Numerical simulations of optically thick accretion onto a black hole. I. Spherical case. United States: N. p., 2012. Web. doi:10.1088/0067-0049/201/2/9.
Fragile, P. Chris, Gillespie, Anna, Monahan, Timothy, Rodriguez, Marco, & Anninos, Peter. Numerical simulations of optically thick accretion onto a black hole. I. Spherical case. United States. doi:10.1088/0067-0049/201/2/9.
Fragile, P. Chris, Gillespie, Anna, Monahan, Timothy, Rodriguez, Marco, and Anninos, Peter. Fri . "Numerical simulations of optically thick accretion onto a black hole. I. Spherical case". United States. doi:10.1088/0067-0049/201/2/9. https://www.osti.gov/servlets/purl/1564878.
@article{osti_1564878,
title = {Numerical simulations of optically thick accretion onto a black hole. I. Spherical case},
author = {Fragile, P. Chris and Gillespie, Anna and Monahan, Timothy and Rodriguez, Marco and Anninos, Peter},
abstractNote = {Modeling the radiation generated by accreting matter is an important step toward realistic simulations of black hole accretion disks, especially at high accretion rates. To this end, we have recently added radiation transport to the existing general relativistic magnetohydrodynamic code, Cosmos++. However, before attempting to model radiative accretion disks, we have tested the new code using a series of shock tube and Bondi (spherical inflow) problems. The four radiative shock tube tests, first presented by Farris et al., have known analytic solutions, allowing us to calculate errors and convergence rates for our code. The Bondi problem only has an analytic solution when radiative processes are ignored, but it is pertinent because it is closer to the physics we ultimately want to study. In our simulations, we include Thomson scattering and thermal bremsstrahlung in the opacity, focusing exclusively on the super-Eddington regime. Unlike accretion onto bodies with solid surfaces, super-Eddington accretion onto black holes does not produce super-Eddington luminosity. In our examples, despite accreting at up to 300 times the Eddington rate, our measured luminosity is always several orders of magnitude below Eddington.},
doi = {10.1088/0067-0049/201/2/9},
journal = {Astrophysical Journal, Supplement Series},
number = 2,
volume = 201,
place = {United States},
year = {2012},
month = {6}
}

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