Bipolar supernova remnants and the obliquity dependence of shock acceleration

Details Bipolar supernova remnants and the obliquity dependence of shock acceleration Bipolar supernova remnants and the obliquity dependence of shock acceleration

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...357..591f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 357, July 10, 1990, p. 591-601.

Statistics

Computation

46

Oblique Shock Waves, Particle Acceleration, Relativistic Electron Beams, Supernova Remnants, Synchrotron Radiation, Energetic Particles, Flux Density, Line Of Sight, Magnetic Field Configurations

Scientific paper

The diffusive shock acceleration mechanism proposed to explain the bipolarity observed in the synchrotron radio emission of young adiabatically expanding shell SNRs is investigated by means of numerical simulations. The theoretical basis of the SNR models and the numerical computation methods are explained, and the results are presented in graphs and synthetic radio maps and discussed in detail. It is found that the efficiency of the acceleration process depends on the obliquity angle theta(Bn) between the shock normal and the uniform magnetic field: models with theta(Bn) of about 90 deg can reproduce the observed azimuthal intensity ratios in most cases, but models with theta(Bn) near 0 deg cannot.

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