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Title: Two-temperature GRRMHD Simulations of M87

Abstract

Here, we present axisymmetric two-temperature general relativistic radiation magnetohydrodynamic simulations of the inner region of the accretion flow onto the supermassive black hole M87. We address uncertainties from previous modeling efforts through inclusion of models for (1) self-consistent dissipative and Coulomb electron heating (2) radiation transport (3) frequency-dependent synchrotron emission, self-absorption, and Compton scattering. We adopt a distance D = 16.7 Mpc, an observer angle θ = 20°, and consider black hole masses M/M = (3.3 x 10 9, 6.2 x 10 9) and spins a star = (0.5, 0.9375) in a four-simulation suite. For each (M, a star), we identify the accretion rate that recovers the 230 GHz flux from very long baseline interferometry measurements. We report on disk thermodynamics at these accretion rates (M ·/M · Edd ~ 10 -5). The disk remains geometrically thick; cooling does not lead to a thin disk component. While electron heating is dominated by Coulomb rather than dissipation for r ≳ 10GM/c 2, the accretion disk remains two-temperature. Radiative cooling of electrons is not negligible, especially for r ≲ 10GM/c 2. The Compton y parameter is of order unity. We then compare derived and observed or inferred spectra, millimeter images, andmore » jet powers. Simulations with M/M = 3.3 × 10 9 are in conflict with observations. These simulations produce millimeter images that are too small, while the low-spin simulation also overproduces X-rays. For M/M = 6.2 x 10 9, both simulations agree with constraints on radio/IR/X-ray fluxes and millimeter image sizes. Simulation jet power is a factor 10 2–10 3 below inferred values, a possible consequence of the modest net magnetic flux in our models.« less

Authors:
ORCiD logo [1]; ORCiD logo [2];  [1]; ORCiD logo [3]; ORCiD logo [2]
  1. Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  2. Univ. of California, Berkeley, CA (United States). Dept. of Astronomy. Dept. of Physics. Theoretical Astrophysics Center
  3. Univ. of Illinois, Urbana, IL (United States). Dept. of Astronomy. Dept. of Physics
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Univ. of California, Berkeley, CA (United States); Univ. of Illinois at Urbana-Champaign, IL (United States)
Sponsoring Org.:
USDOE National Nuclear Security Administration (NNSA); LANL Laboratory Directed Research and Development (LDRD) Program; National Aeronautic and Space Administration (NASA); National Science Foundation (NSF); Smithsonian Institution (United States); Simons Foundation (United States)
OSTI Identifier:
1479992
Report Number(s):
[LA-UR-18-23675]
[Journal ID: ISSN 1538-4357]
Grant/Contract Number:  
[AC52-06NA25396; AST 13-33612; AST 1715054; ACI-1053575; TM7-18006X]
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
[Journal Name: The Astrophysical Journal (Online); Journal Volume: 864; Journal Issue: 2]; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; accretion; accretion disks; magnetohydrodynamics (MHD); plasmas; radiation dynamics; radiative transfer; turbulence

Citation Formats

Ryan, Benjamin R., Ressler, Sean M., Dolence, Joshua C., Gammie, Charles, and Quataert, Eliot. Two-temperature GRRMHD Simulations of M87. United States: N. p., 2018. Web. doi:10.3847/1538-4357/aad73a.
Ryan, Benjamin R., Ressler, Sean M., Dolence, Joshua C., Gammie, Charles, & Quataert, Eliot. Two-temperature GRRMHD Simulations of M87. United States. doi:10.3847/1538-4357/aad73a.
Ryan, Benjamin R., Ressler, Sean M., Dolence, Joshua C., Gammie, Charles, and Quataert, Eliot. Fri . "Two-temperature GRRMHD Simulations of M87". United States. doi:10.3847/1538-4357/aad73a. https://www.osti.gov/servlets/purl/1479992.
@article{osti_1479992,
title = {Two-temperature GRRMHD Simulations of M87},
author = {Ryan, Benjamin R. and Ressler, Sean M. and Dolence, Joshua C. and Gammie, Charles and Quataert, Eliot},
abstractNote = {Here, we present axisymmetric two-temperature general relativistic radiation magnetohydrodynamic simulations of the inner region of the accretion flow onto the supermassive black hole M87. We address uncertainties from previous modeling efforts through inclusion of models for (1) self-consistent dissipative and Coulomb electron heating (2) radiation transport (3) frequency-dependent synchrotron emission, self-absorption, and Compton scattering. We adopt a distance D = 16.7 Mpc, an observer angle θ = 20°, and consider black hole masses M/M⊙ = (3.3 x 109, 6.2 x 109) and spins astar = (0.5, 0.9375) in a four-simulation suite. For each (M, astar), we identify the accretion rate that recovers the 230 GHz flux from very long baseline interferometry measurements. We report on disk thermodynamics at these accretion rates (M·/M·Edd ~ 10-5). The disk remains geometrically thick; cooling does not lead to a thin disk component. While electron heating is dominated by Coulomb rather than dissipation for r ≳ 10GM/c 2, the accretion disk remains two-temperature. Radiative cooling of electrons is not negligible, especially for r ≲ 10GM/c 2. The Compton y parameter is of order unity. We then compare derived and observed or inferred spectra, millimeter images, and jet powers. Simulations with M/M ⊙ = 3.3 × 109 are in conflict with observations. These simulations produce millimeter images that are too small, while the low-spin simulation also overproduces X-rays. For M/M⊙ = 6.2 x 109, both simulations agree with constraints on radio/IR/X-ray fluxes and millimeter image sizes. Simulation jet power is a factor 102–103 below inferred values, a possible consequence of the modest net magnetic flux in our models.},
doi = {10.3847/1538-4357/aad73a},
journal = {The Astrophysical Journal (Online)},
number = [2],
volume = [864],
place = {United States},
year = {2018},
month = {9}
}

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