Ion and electron heating at the low-Mach-number, quasi-parallel bow shock

1993 ◽  
Vol 98 (A3) ◽  
pp. 3875-3888 ◽  
Author(s):  
M. F. Thomsen ◽  
J. T. Gosling ◽  
T. G. Onsager ◽  
C. T. Russell
Keyword(s):  
Mach Number ◽  
Bow Shock ◽  
Electron Heating ◽  
Low Mach Number

Kinetic simulations of high Mach shocks: PIC simulations vs in-situ measurements

2021 ◽  
Author(s):  
Artem Bohdan ◽  
Martin Pohl ◽  
Jacek Niemiec ◽  
Paul J. Morris ◽  
Yosuke Matsumoto ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Mach Number ◽  
Supernova Remnants ◽  
Large Scale ◽  
Bow Shock ◽  
Electron Heating ◽  
Weibel Instability ◽  
High Mach Number ◽  
High Mach

<p>High-Mach-number collisionless shocks are found in planetary systems and supernova remnants (SNRs). Electrons are heated at these shocks to temperatures well above the Rankine–Hugoniot prediction. However, the processes responsible for causing the electron heating are still not well understood. We use a set of large-scale particle-in-cell simulations of nonrelativistic shocks in the high-Mach-number regime to clarify the electron heating processes. The physical behavior of these shocks is defined by ion reflection at the shock ramp. Further interactions between the reflected ions and the upstream plasma excites electrostatic Buneman and two-stream ion–ion Weibel instabilities. Electrons are heated via shock surfing acceleration, the shock potential, magnetic reconnection, stochastic Fermi scattering, and shock compression. The main contributor is the shock potential. The magnetic field lines become tangled due to the Weibel instability, which allows for parallel electron heating by the shock potential. The constrained model of electron heating predicts an ion-to-electron temperature ratio within observed values at SNR shocks and in Saturn’s bow shock. We also present evidence for field amplification by the Weibel instability. The normalized magnetic field strength strongly correlates with the Alfvenic Mach number, as is in-situ observed at Saturn's bow shock.</p>

scholarly journals A statistical study of the cross-shock electric potential at low Mach number, quasi-perpendicular bow shock crossings using Cluster data

2012 ◽  
Vol 117 (A2) ◽  
pp. n/a-n/a ◽  
Author(s):  
A. P. Dimmock ◽  
M. A. Balikhin ◽  
V. V. Krasnoselskikh ◽  
S. N. Walker ◽  
S. D. Bale ◽  
...  
Keyword(s):  
Mach Number ◽  
Electric Potential ◽  
Statistical Study ◽  
Bow Shock ◽  
Low Mach Number ◽  
Cluster Data ◽  
The Cross

scholarly journals Electron Heating in Low-Mach-number Perpendicular Shocks. I. Heating Mechanism

2017 ◽  
Vol 851 (2) ◽  
pp. 134 ◽  
Author(s):  
Xinyi Guo ◽  
Lorenzo Sironi ◽  
Ramesh Narayan
Keyword(s):  
Mach Number ◽  
Electron Heating ◽  
Low Mach Number ◽  
Heating Mechanism

scholarly journals The role of the bow shock in solar wind-magnetosphere coupling

2011 ◽  
Vol 29 (6) ◽  
pp. 1129-1135 ◽  
Author(s):  
R. E. Lopez ◽  
V. G. Merkin ◽  
J. G. Lyon
Keyword(s):  
Solar Wind ◽  
Mach Number ◽  
High Latitude ◽  
Mechanical Energy ◽  
Bow Shock ◽  
Low Mach Number ◽  
Poynting Flux ◽  
Wind Speeds ◽  
Magnetohydrodynamic Simulations

Abstract. In this paper we examine the role of the bow shock in coupling solar wind energy to the magnetosphere using global magnetohydrodynamic simulations of the solar wind-magnetosphere interaction with southward IMF. During typical solar wind conditions, there are two significant dynamo currents in the magnetospheric system, one in the high-latitude mantle region tailward of the cusp and the other in the bow shock. As the magnitude of the (southward) IMF increases and the solar wind becomes a low Mach number flow, there is a significant change in solar wind-magnetosphere coupling. The high-latitude magnetopause dynamo becomes insignificant compared to the bow shock and a large load appears right outside the magnetopause. This leaves the bow shock current as the only substantial dynamo current in the system, and the only place where a significant amount of mechanical energy is extracted from the solar wind. That energy appears primarily as electromagnetic energy, and the Poynting flux generated at the bow shock feeds energy back into the plasma, reaccelerating it to solar wind speeds. Some small fraction of that Poynting flux is directed into the magnetosphere, supplying the energy needed for magnetospheric dynamics. Thus during periods when the solar wind flow has a low Mach number, the main dynamo in the solar wind-magnetosphere system is the bow shock.

A study of kinematic relaxation at the Venus bow shock

2020 ◽  
Author(s):  
Simon A. Pope ◽  
Michael A. Balikhin
Keyword(s):  
Magnetic Field ◽  
Mach Number ◽  
Heavy Ions ◽  
Magnetic Cloud ◽  
Bow Shock ◽  
Primary Method ◽  
Low Mach Number ◽  
The Earth ◽  
New Type ◽  
Venus Express

<p>A new type of very-low Mach number shock in which the primary method of energy re-distribution is the kinematic relaxation of a non-gyrotropic ion population, was discovered at Venus early in the Venus Express mission. This led to the development of an associated theory and numerical analysis. The recent discovery of such a shock at the Earth using THEMIS data experimentally verified this theory using simultaneous magnetic field and plasma data. It also showed that the most favourable conditions for the formation of such a shock is the magnetic cloud phase of an ICME. Venus Express provides an excellent opportunity to study such shocks further. Here we present results from the duration of the mission, which identifies over thirty shock crossings showing evidence of kinematic relaxation. These shock crossings are investigated to understand how the upstream conditions and heavy ions (including pick-up ions) affect their formation.</p>

Electron heating by ion acoustic turbulence in simulated low Mach number shocks

1987 ◽  
Vol 30 (8) ◽  
pp. 2569 ◽  
Author(s):  
Robert L. Tokar ◽  
S. Peter Gary ◽  
Kevin B. Quest
Keyword(s):  
Mach Number ◽  
Electron Heating ◽  
Low Mach Number ◽  
Ion Acoustic

scholarly journals Low Mach number fluctuating hydrodynamics for electrolytes

2016 ◽  
Vol 1 (7) ◽  
Author(s):  
Jean-Philippe Péraud ◽  
Andy Nonaka ◽  
Anuj Chaudhri ◽  
John B. Bell ◽  
Aleksandar Donev ◽  
...  
Keyword(s):  
Mach Number ◽  
Fluctuating Hydrodynamics ◽  
Low Mach Number
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