Electron Heating at Supernova Remnant Collisionless Shocks

2000 ◽  
Vol 127 (2) ◽  
pp. 409-413 ◽  
Author(s):  
J. Martin Laming
Keyword(s):  
Supernova Remnant ◽  
Collisionless Shocks ◽  
Electron Heating

scholarly journals ELECTRON HEATING, MAGNETIC FIELD AMPLIFICATION, AND COSMIC-RAY PRECURSOR LENGTH AT SUPERNOVA REMNANT SHOCKS

2014 ◽  
Vol 790 (1) ◽  
pp. 11 ◽  
Author(s):  
J. Martin Laming ◽  
Una Hwang ◽  
Parviz Ghavamian ◽  
Cara Rakowski
Keyword(s):  
Magnetic Field ◽  
Supernova Remnant ◽  
Cosmic Ray ◽  
Electron Heating ◽  
Field Amplification

scholarly journals Electron-Ion Temperature Equilibration in Collisionless Shocks: The Supernova Remnant-Solar Wind Connection

2013 ◽  
Vol 178 (2-4) ◽  
pp. 633-663 ◽  
Author(s):  
Parviz Ghavamian ◽  
Steven J. Schwartz ◽  
Jeremy Mitchell ◽  
Adam Masters ◽  
J. Martin Laming
Keyword(s):  
Solar Wind ◽  
Supernova Remnant ◽  
Ion Temperature ◽  
Collisionless Shocks

scholarly journals Diffusive shock re-acceleration

2018 ◽  
Vol 84 (3) ◽  
Author(s):  
Damiano Caprioli ◽  
Horace Zhang ◽  
Anatoly Spitkovsky
Keyword(s):  
Magnetic Field ◽  
Supernova Remnant ◽  
Galactic Cosmic Rays ◽  
Energetic Particles ◽  
Clusters Of Galaxies ◽  
Minimum Level ◽  
Collisionless Shocks ◽  
Field Amplification ◽  
Streaming Instability ◽  
Oblique Shocks

We have performed two-dimensional hybrid simulations of non-relativistic collisionless shocks in the presence of pre-existing energetic particles (‘seeds’); such a study applies, for instance, to the re-acceleration of galactic cosmic rays (CRs) in supernova remnant (SNR) shocks and solar wind energetic particles in heliospheric shocks. Energetic particles can be effectively reflected and accelerated regardless of shock inclination via a process that we call diffusive shock re-acceleration. We find that re-accelerated seeds can drive the streaming instability in the shock upstream and produce effective magnetic field amplification. This can eventually trigger the injection of thermal protons even at oblique shocks that ordinarily cannot inject thermal particles. We characterize the current in reflected seeds, finding that it tends to a universal value $J\simeq en_{\text{CR}}v_{\text{sh}}$, where $en_{\text{CR}}$ is the seed charge density and $v_{\text{sh}}$ is the shock velocity. When applying our results to SNRs, we find that the re-acceleration of galactic CRs can excite the Bell instability to nonlinear levels in less than ${\sim}10~\text{yr}$, thereby providing a minimum level of magnetic field amplification for any SNR shock. Finally, we discuss the relevance of diffusive shock re-acceleration also for other environments, such as heliospheric shocks, galactic superbubbles and clusters of galaxies.

Ion and electron heating at collisionless shocks near the critical Mach number

1985 ◽  
Vol 90 (A1) ◽  
pp. 137-148 ◽  
Author(s):  
M. F. Thomsen ◽  
J. T. Gosling ◽  
S. J. Bame ◽  
M. M. Mellott
Keyword(s):  
Mach Number ◽  
Collisionless Shocks ◽  
Electron Heating ◽  
Critical Mach Number

scholarly journals Particle simulation study of electron heating by counter-streaming ion beams ahead of supernova remnant shocks

2012 ◽  
Vol 54 (8) ◽  
pp. 085015 ◽  
Author(s):  
M E Dieckmann ◽  
A Bret ◽  
G Sarri ◽  
E Perez Alvaro ◽  
I Kourakis ◽  
...  
Keyword(s):  
Simulation Study ◽  
Supernova Remnant ◽  
Ion Beams ◽  
Particle Simulation ◽  
Electron Heating
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