Physics – Plasma Physics
Scientific paper
Oct 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..dppgp1147s&link_type=abstract
American Physical Society, 45th Annual Meeting of the Division of Plasma Physics, October 27-31, 2003, Albuquerque, New Mexico,
Physics
Plasma Physics
Scientific paper
The cosmic rays are believed to be accelerated by the Fermi Class I mechanism at supernova remnants. A crucial ingredient in this mechanism is the presence of wave turbulence upstream and downstream of the supernova remnant shock. The point of this paper is to emphasize that the upstream turbulence, generated by cosmic ray streaming, will be enormously amplified by passage through the shock, and will become much more compressive. The amplification is largely a consequence of the shock jump conditions. Increased compressibility is due in part to the fact that dynamically aligned upstream turbulence will no longer be so after passage through the shock, leading to strong nonlinear evolution. In addition, even for unidirectionally-propagating waves upstream, a mixture of counterpropagating waves will exist downstream. This mixture of bidirectionally-propagating waves will generate density compressions via the parametric decay instability of MHD waves. I will describe the status of radioastronomical observations to test these theoretical ideas. The level of turbulence in a supernova remnant can be measured by the angular broadening or blurring of a radio source viewed through the remnant. In the case of three supernova remnants (G127.1+0.5, S147, and the Cygnus Loop) there appears to be evidence of anomalous broadening. I will present recent results from highly improved observations for the first two remnants.
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