Computer Science
Scientific paper
Aug 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aipc..264..313a&link_type=abstract
In: Particle acceleration in cosmic plasmas; Proceedings of the Workshop, Bartol Research Inst., Newark, DE, Dec. 4-6, 1991 (A93
Computer Science
3
Magnetoacoustic Waves, Particle Acceleration, Pulsars, Relativistic Plasmas, Shock Wave Interaction, Supernova Remnants, Magnetohydrodynamic Waves, Stellar Winds
Scientific paper
Results on the structure of relativistic magnetosonic shock waves in plasmas composed of electrons and positrons plus heavy ions as a minority constituent by number are described. In a specific model presented in some detail, s = 1.7, with approximately 20 percent efficiency in converting upstream flow energy into downstream energy in nonthermally accelerated particles. The acceleration mechanism is collective synchrotron emission of elliptically polarized extraordinary modes by the ions in the shock front at high harmonics of the ion cyclotron frequency, with the downstream pairs absorbing almost all of this radiation, mostly at their fundamental (relativistic) cyclotron frequencies. A new model of the inner regions of the Crab Nebula is outlined; it is proposed that the shock structure is angularly resolved and the optical 'wisps' are surface brightness enhancements created in the compressional overshoots of the magnetic field within and just downstream from the shock.
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