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Fundamentals of collisionless shocks for astrophysical application, 1. Non-relativistic shocks

Treumann, R. A. (2009), Fundamentals of collisionless shocks for astrophysical application, 1. Non-relativistic shocks, Astronomy & Astrophysics Reviews, 17(4), 409-535, doi:10.1007/s00159-009-0024-2.

Abstract
Abstract A comprehensive review is given of the theory and properties of nonrelativistic
shocks in hot collisionless plasmas in view of their possible application in astrophysics. Understanding
non-relativistic collisionless shocks is an indispensable step towards a general
account of high-Mach number collisionless astrophysical shocks and their effects in dissipating
flow energy, heating matter, accelerating particles to high – presumably cosmic ray –
energies, and generation of detectable radiation from radio to x-rays. Non-relativistic shocks
have low Alfv´enic Mach numbers MA pmi=me(wpe=wce), with mi=me ion-to-electron
mass ratio, and wpe;wce the electron plasma and cyclotron frequencies, respectively. Though
of high temperature, their temperatures (in energy units) are limited to T < mec2, such
that particle creation is inhibited, classical theory is applicable, and reaction of radiation
on the dynamics of the shock can be neglected. The majority of such shocks is supercritical,
i.e. they are unable to self-consistently produce sufficient dissipation for sustaining a
stationary shock. As a consequence, they act as strong particle reflectors. All these shocks
are microscopically thin, with shock-transition width of the order of the ion inertial length
li = c=wpi. The full theory of these shocks is developed, and the different possible types of
shocks are defined. Since all collisionless shocks are magnetised, the most important distinction
is between quasi-perpendicular and quasi-parallel shocks. The former propagate about
perpendicular, the latter about parallel to the upstream magnetic field. Their manifestly different
behaviour is described in detail. In particular, both types of shocks are non-stationary
with completely different reformation cycles. From numerical full-particle simulations it
becomes evident that, on ion-inertial scales close to the shock transition, quasi-parallel collisionless
supercritical shocks behave locally quasi-perpendicular. This property is of vital
importance for the particle dynamics near the quasi-parallel shock front. Considerable interest
focusses on particle acceleration and the generation of radiation. Radiation from nonrelativistic
shocks results mainly in wave-wave interactions among various plasma waves.
Non-thermal charged particles can be further accelerated to high energies by a Fermi-like
mechanism. The important question is, whether the shock can pre-accelerate shock-reflected
particles to sufficiently high energies in order to create the seed-population of non-thermal
particles which the Fermi mechanism requires. Based on preliminary full-particle numerical
simulations this question is answered affirmatively. Such simulations provide evidence for
the capability of high-Mach number collisionless shocks, even when being non-relativistic,
of producing the seed population for the Fermi-process.

Keywords: Collisionless shocks - Supercritical shocks - Shock kinetics - Shock reformation - Shock acceleration
PACS Numbers: 95.30.Qd, 52.35.Tc, 52.72.+v
BibTeX
@article{id1407,
  author = {R. A. Treumann},
  journal = {Astronomy {\&} Astrophysics Reviews},
  month = {aug},
  number = {4},
  pages = {409-535},
  title = {{Fundamentals of collisionless shocks for astrophysical application, 1. Non-relativistic shocks}},
  volume = {17},
  year = {2009},
  doi = {10.1007/s00159-009-0024-2},
}
EndNote
%0 Journal Article
%A Treumann, R. A.
%D 2009
%N 4
%V 17
%J Astronomy & Astrophysics Reviews
%P 409-535
%T Fundamentals of collisionless shocks for astrophysical application, 1. Non-relativistic shocks
%8 aug
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