Electron Heating in Low-Mach-number Perpendicular Shocks. I. Heating Mechanism
Abstract
Recent X-ray observations of merger shocks in galaxy clusters have shown that the postshock plasma has two temperatures, with the protons hotter than the electrons. By means of two-dimensional particle-in-cell simulations, we study the physics of electron irreversible heating in low-Mach-number perpendicular shocks, for a representative case with sonic Mach number of 3 and plasma beta of 16. We find that two basic ingredients are needed for electron entropy production: (1) an electron temperature anisotropy, induced by field amplification coupled to adiabatic invariance; and (2) a mechanism to break the electron adiabatic invariance itself. In shocks, field amplification occurs at two major sites: at the shock ramp, where density compression leads to an increase of the frozen-in field; and farther downstream, where the shock-driven proton temperature anisotropy generates strong proton cyclotron and mirror modes. The electron temperature anisotropy induced by field amplification exceeds the threshold of the electron whistler instability. The growth of whistler waves breaks the electron adiabatic invariance and allows for efficient entropy production. For our reference run, the postshock electron temperature exceeds the adiabatic expectation by $$\simeq 15 \% $$, resulting in an electron-to-proton temperature ratio of $$\simeq 0.45$$. We find that the electron heating efficiency displays only a weak dependence on mass ratio (less than $$\simeq 30 \% $$ drop, as we increase the mass ratio from $${m}_{i}/{m}_{e}=49$$ up to $${m}_{i}/{m}_{e}=1600$$). We develop an analytical model of electron irreversible heating and show that it is in excellent agreement with our simulation results.
- Authors:
-
[1];
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
- Columbia Univ., New York, NY (United States)
- Publication Date:
- Research Org.:
- Columbia Univ., New York, NY (United States)
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 1511008
- Grant/Contract Number:
- SC0016542
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 851; 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
Citation Formats
Guo, Xinyi, Sironi, Lorenzo, and Narayan, Ramesh. Electron Heating in Low-Mach-number Perpendicular Shocks. I. Heating Mechanism. United States: N. p., 2017.
Web. doi:10.3847/1538-4357/aa9b82.
Guo, Xinyi, Sironi, Lorenzo, & Narayan, Ramesh. Electron Heating in Low-Mach-number Perpendicular Shocks. I. Heating Mechanism. United States. https://doi.org/10.3847/1538-4357/aa9b82
Guo, Xinyi, Sironi, Lorenzo, and Narayan, Ramesh. Wed .
"Electron Heating in Low-Mach-number Perpendicular Shocks. I. Heating Mechanism". United States. https://doi.org/10.3847/1538-4357/aa9b82. https://www.osti.gov/servlets/purl/1511008.
@article{osti_1511008,
title = {Electron Heating in Low-Mach-number Perpendicular Shocks. I. Heating Mechanism},
author = {Guo, Xinyi and Sironi, Lorenzo and Narayan, Ramesh},
abstractNote = {Recent X-ray observations of merger shocks in galaxy clusters have shown that the postshock plasma has two temperatures, with the protons hotter than the electrons. By means of two-dimensional particle-in-cell simulations, we study the physics of electron irreversible heating in low-Mach-number perpendicular shocks, for a representative case with sonic Mach number of 3 and plasma beta of 16. We find that two basic ingredients are needed for electron entropy production: (1) an electron temperature anisotropy, induced by field amplification coupled to adiabatic invariance; and (2) a mechanism to break the electron adiabatic invariance itself. In shocks, field amplification occurs at two major sites: at the shock ramp, where density compression leads to an increase of the frozen-in field; and farther downstream, where the shock-driven proton temperature anisotropy generates strong proton cyclotron and mirror modes. The electron temperature anisotropy induced by field amplification exceeds the threshold of the electron whistler instability. The growth of whistler waves breaks the electron adiabatic invariance and allows for efficient entropy production. For our reference run, the postshock electron temperature exceeds the adiabatic expectation by $\simeq 15 \% $, resulting in an electron-to-proton temperature ratio of $\simeq 0.45$. We find that the electron heating efficiency displays only a weak dependence on mass ratio (less than $\simeq 30 \% $ drop, as we increase the mass ratio from ${m}_{i}/{m}_{e}=49$ up to ${m}_{i}/{m}_{e}=1600$). We develop an analytical model of electron irreversible heating and show that it is in excellent agreement with our simulation results.},
doi = {10.3847/1538-4357/aa9b82},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 851,
place = {United States},
year = {Wed Dec 20 00:00:00 EST 2017},
month = {Wed Dec 20 00:00:00 EST 2017}
}
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