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| Title: |
| Oblique MHD shocks: space-like and time-like |
| Authors: |
| Mallick, Ritam; Schramm, Stefan |
| Publication: |
| eprint arXiv:1309.0397 |
| Publication Date: |
| 09/2013 |
| Origin: |
| ARXIV |
| Keywords: |
| Astrophysics - High Energy Astrophysical Phenomena |
| Comment: |
| 20 pages, 6 figures |
| Bibliographic Code: |
| 2013arXiv1309.0397M |
Abstract
Shock waves constitute discontinuities in matter which are relevant in
studying the plasma
behaviour in astrophysical scenarios and in
heavy-ion collision. They can produce conical emission in relativistic
collisions and are also thought to be the mechanism behind the
acceleration of energetic particles in active galactic nuclei and gamma
ray bursts. The shocks are mostly hydrodynamic shocks. In a magnetic
background they become magnetohydrodynamic (MHD) shocks. For that reason
we study the space-like and time-like shock discontinuity in a magnetic
plasma. The shocks induce a phase transition in the plasma,
here
assuming a transition from
hadron to quarks. The MHD conservation
conditions are derived across the shock. The conservation conditions are
solved for downstream velocities and flow angles for
given upstream
variables. The shock conditions are solved at different baryon
densities. For the space-
like shocks the anisotropy in the downstream
velocity arises due to the magnetic field. The downstream velocity
vector always points downward with respect to the
shock normal. With the
increase in density the anisotropy is somewhat reduced. The magnetic
field has effectively no effect on
time-like shocks. The slight
anisotropy in the downstream flow velocities is caused by the boosting
that brings the quantities from the fluid frame to normal incidence (NI)
frame.
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