Kinetic Simulations of Nonrelativistic Perpendicular Shocks of Young Supernova Remnants. I. Electron Shock-surfing Acceleration

Electron injection at high Mach number nonrelativistic perpendicular shocks is studied here for parameters that are applicable to young SNR shocks. Using high-resolution large-scale two-dimensional fully kinetic particle-in-cell simulations and tracing individual particles, we in detail analyze the...

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Bibliographic Details
Published in:The Astrophysical journal 2019-06, Vol.878 (1), p.5
Main Authors: Bohdan, Artem, Niemiec, Jacek, Pohl, Martin, Matsumoto, Yosuke, Amano, Takanobu, Hoshino, Masahiro
Format: Article
Language:English
Subjects:
Acceleration
acceleration of particles
Activation
Astrophysics
Electric fields
Electrons
High Mach number
instabilities
ISM: supernova remnants
Mach number
Magnetic fields
methods: numerical
Parameter modification
Particle in cell technique
Phase velocity
plasmas
shock waves
Simulation
Supernova
Supernova remnants
Surfing
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Summary:Electron injection at high Mach number nonrelativistic perpendicular shocks is studied here for parameters that are applicable to young SNR shocks. Using high-resolution large-scale two-dimensional fully kinetic particle-in-cell simulations and tracing individual particles, we in detail analyze the shock-surfing acceleration (SSA) of electrons at the leading edge of the shock foot. The central question is to what degree the process can be captured in 2D3V simulations. We find that the energy gain in SSA always arises from the electrostatic field of a Buneman wave. Electron energization is more efficient in the out-of-plane orientation of the large-scale magnetic field because both the phase speed and the amplitude of the waves are higher than for the in-plane scenario. Also, a larger number of electrons is trapped by the waves compared to the in-plane configuration. We conclude that significant modifications of the simulation parameters are needed to reach the same level of SSA efficiency as in simulations with out-of-plane magnetic field or 3D simulations.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ab1b6d