Physics
Scientific paper
Aug 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....6.2022s&link_type=abstract
Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int
Physics
2
Scientific paper
Electron pre-acceleration from thermal to mildly relativistic energies in high Mach number shocks (the injection problem) is an outstanding issue in understanding synchrotron radiation from supernova remnants. At high Alfv´enic Mach numbers, collisionless perpendicular shocks reflect a fraction of the upstream ions. This gives rise to two-stream instabilities which in turn can accelerate ions, see eg (M. E. Dieckmann et al., Astron. Astrophys. 356, 377 (2000)). However in astrophysical plasmas the value of β - the ratio of kinetic to magnetic pressure - is not well known. We have used a particle in cell simulation code to investigate the influence of β on the shock structure and on the electron acceleration. Previous simulations at low values of β (N. Shimada and M. Hoshino, Astrophys. J. 543, L67 (2000)) showed that the phase space distributions of electrons and ions became highly structured: characteristic holes appear in the electron phase space and the shock dynamics exhibit reformation processes. However, we find that all these features disappear at higher β due to the high initial thermal velocity of the electrons. It follows that the electron cosmic ray injection mechanism depends strongly on β, that is, the electron temperature and magnetic field strength upstream.
Chapman Sandra C.
Dendy R. O.
Schmitz Heiko
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