Electron Thermodynamics in GRMHD Simulations of Low-Luminosity Black Hole Accretion

By S. Ressler, A. Tchekhovskoy, E. Quataert, M. Chandra, Charles F. Gammie. 2015

148 citations recorded by the source corpus.

Simple assumptions made regarding electron thermodynamics often limit the extent to which general relativistic magnetohydrodynamic (GRMHD) simulations can be applied to observations of low-luminosity accreting black holes. We present, implement, and test a model that self-consistently evolves an electron entropy equation and takes into account the effects of spatially varying electron heating and relativistic anisotropic thermal conduction along magnetic field lines. We neglect the back-reaction of electron pressure on the dynamics of the accretion flow. Our model is appropriate for systems accreting at $\ll 10^{-5}$ of the Eddington rate, so radiative cooling by electrons can be neglected. It can be extended to higher accretion rates in the future by including electron cooling and proton-electron Coulomb collisions. We present a suite of tests showing that our method recovers the correct solution for electron heating under a range of circumstances, including strong shocks and driven turbulence. Our initial applications to axisymmetric simulations of accreting black holes show that (1)~physically-motivated electron heating rates yield electron temperature distributions significantly different from the constant electron to proton temperature ratios assumed in previous work, with higher electron temperatures concentrated in the coronal region between the disc and the jet; (2)~electron thermal conduction significantly modifies the electron temperature in the inner regions of black hole accretion flows if the effective electron mean free path is larger than the local scale-height of the disc (at least for the initial conditions and magnetic field configurations we study). The methods developed in this work are important for producing more realistic predictions for the emission from accreting black holes such as Sagittarius A* and M87; these applications will be explored in future work.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5ad4d37027c085d62f82a2633b29a63ec4534b07

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Citations in the corpus

First Sagittarius A* Event Horizon Telescope Results. V. Testing Astrophysical Models of the Galactic Center Black Hole (2022, methodology): “Effect of Self-consistent Electron Heating Ressler et al. (2015) provide a formulation to model electron thermodynamics during the fluid evolution.”
First M87 Event Horizon Telescope Results. V. Physical Origin of the Asymmetric Ring (2019, unknown): “…dissipation into the electrons and ions, as well as heating and cooling physics that sets the temperature ratio Ti/Te, have been added to GRMHD and radiative GRMHD codes and used in simulations of Sgr A* (Ressler et al. 2015, 2017; Chael et al. 2018) and M87 (Ryan et al. 2018; Chael et al. 2019).”
Black Hole Flares: Ejection of Accreted Magnetic Flux through 3D Plasmoid-mediated Reconnection (2021, background): “…Collaboration et al. 2019b; Dexter et al. 2020; Yoon et al. 2020; Chatterjee et al. 2021, and references therein) or two-temperature GRMHD approaches (Ressler et al. 2015; Chael et al. 2019) therefore cannot describe the nonthermal emission from these events, which involves reconnection in high-σ…”
Non-thermal particle acceleration in collisionless relativistic electron-proton reconnection (2016, background): “(3) This electron heating fraction, as a function of σi, may potentially serve as a physically motivated prescription for calculating radiative signatures of small-scale reconnection in global MHD simulations of black holes (e.g., Ressler et al. 2015).”