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 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 ×more »
- Authors:
-
[1];
[2];
[3];
[2]
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- Univ. of California, Berkeley, CA (United States). Dept. of Astronomy. Dept. of Physics. Theoretical Astrophysics Center
- 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 Aeronautics 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. https://doi.org/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. https://doi.org/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 = {Fri Sep 07 00:00:00 EDT 2018},
month = {Fri Sep 07 00:00:00 EDT 2018}
}
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- arXiv
Radiative Models of Sgr A* from GRMHD Simulations
text, January 2009
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- arXiv
Fermi Large Area Telescope Gamma-Ray Detection of the Radio Galaxy M87
text, January 2009
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- arXiv
Binary Black Hole Mergers in Gaseous Environments: "Binary Bondi" and "Binary Bondi-Hoyle-Lyttleton" Accretion
text, January 2009
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- arXiv
Sagittarius A* Accretion Flow and Black Hole Parameters from General Relativistic Dynamical and Polarized Radiative Modeling
text, January 2010
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- arXiv
Radially Extended, Stratified, Local Models of Isothermal Disks
text, January 2010
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- arXiv
The Black-Hole Mass in M87 from Gemini/NIFS Adaptive Optics Observations
text, January 2011
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- arXiv
Pair Production in Low Luminosity Galactic Nuclei
text, January 2011
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- arXiv
Global Structure of Three Distinct Accretion Flows and Outflows around Black Holes through Two-Dimensional Radiation-Magnetohydrodynamic Simulations
text, January 2011
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- arXiv
The 2010 very high energy gamma-ray flare & 10 years of multi-wavelength observations of M 87
text, January 2011
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- arXiv
M87 at metre wavelengths: the LOFAR picture
text, January 2012
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- arXiv
Jet Launching Structure Resolved Near the Supermassive Black Hole in M87
text, January 2012
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- arXiv
Submillimeter Quasi-Periodic Oscillations in Magnetically Choked Accretion Flows Models of Sgr A*
text, January 2013
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- arXiv
The subarcsecond mid-infrared view of local active galactic nuclei: I. The N- and Q-band imaging atlas
text, January 2013
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- arXiv
Electron Heating by the Ion Cyclotron Instability in Collisionless Accretion Flows. I. Compression-Driven Instabilities and the Electron Heating Mechanism
text, January 2014
- Sironi, Lorenzo; Narayan, Ramesh
- arXiv
The central parsecs of M87: jet emission and an elusive accretion disc
text, January 2015
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- arXiv
An Extension of the Athena++ Code Framework for GRMHD Based on Advanced Riemann Solvers and Staggered-Mesh Constrained Transport
text, January 2015
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- arXiv
Strongly magnetized accretion discs require poloidal flux
text, January 2016
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- arXiv
Radiative, two-temperature simulations of low luminosity black hole accretion flows in general relativity
text, January 2016
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- arXiv
Magnetorotational Turbulence and Dynamo in a Collisionless Plasma
text, January 2016
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- arXiv
Kinetic and radiative power from optically thin accretion flows
text, January 2017
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- arXiv
Evolving Nonthermal Electrons in Simulations of Black Hole Accretion
text, January 2017
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- arXiv
The Radiative Efficiency and Spectra of Slowly Accreting Black Holes from Two-Temperature GRRMHD Simulations
text, January 2017
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- arXiv
Constraining the Accretion Rate Onto Sagittarius A* Using Linear Polarization
text, January 2000
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- arXiv
Chandra X-ray Imaging and Spectroscopy of the M87 Jet and Nucleus
text, January 2001
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- arXiv
Magnetically Driven Accretion Flows in the Kerr Metric I: Models and Overall Structure
text, January 2003
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- arXiv
The Intrinsic Size of Sagittarius A* from 0.35 cm to 6 cm
text, January 2006
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- arXiv
Thermal and Non-Thermal Infrared Emission from M87
text, January 2006
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- arXiv
Simulating the Emission and Outflows from Accretion Disks
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Advection-Dominated Accretion and the Spectral States of Black Hole X-Ray Binaries: Application to Nova Muscae 1991
text, January 1997
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Particle Heating by Alfvenic Turbulence in Hot Accretion Flows
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Works referencing / citing this record:
Modeling non-thermal emission from the jet-launching region of M 87 with adaptive mesh refinement
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The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project
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- Maryland Shared Open Access Repository
Neutrino emission from BL Lac objects: the role of radiatively inefficient accretion flows
text, January 2018
- Righi, C.; Tavecchio, F.; Inoue, S.
- arXiv
Electron and Proton Heating in Transrelativistic Guide Field Reconnection
text, January 2019
- Rowan, Michael E.; Sironi, Lorenzo; Narayan, Ramesh
- arXiv
The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project
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- Porth, Oliver; Chatterjee, Koushik; Narayan, Ramesh
- arXiv
First M87 Event Horizon Telescope Results. V. Physical Origin of the Asymmetric Ring
text, January 2019
- Collaboration, The Event Horizon Telescope
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