Nonthermal Radio Emission from SNR in the Pre-Sedov Stage of Evolution : Weak Magnetic Approximation

Details Nonthermal Radio Emission from SNR in the Pre-Sedov Stage of Evolution : Weak Magnetic Approximation Nonthermal Radio Emission from SNR in the Pre-Sedov Stage of Evolution : Weak Magnetic Approximation

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pkas...10...15c&link_type=abstract

Publications of the Korean Astronomical Society, vol.10, no.1, p.15-30

Astronomy and Astrophysics

Astronomy

Scientific paper

It has been recognized that the morphologies of the SNRs from the radio observation are "barrel shaped". To investigate the mechanism of the radiation and the physical state of the environments, we have analytically calculated the dynamical structure of the interacting region in the case where the ejectum has a steep power-law density profile( rho ~ r^-n ) and the ambient medium has a shallow power-law density profile( rho ~ r^-s ), assuming that the cosmic rays are isotropically accelerated in the shock wave and the magnetic fields are very weak. The calculated synchrotron radio maps show that the emission from the equator is intense and the emissions from the central and polar regions are less intense. Also the thickness of the shell are strongly dependent on s and weakly on n. The azimuthal intensity ratio alpha increases as the efficiency of the cosmic ray acceleration increases and s decreases. We compared the results with the morphology of the SNR A.D.1006(type I SNR). It does agree with the case of s=0, w=0.3 - 0.5. This value for w is consistent with the results by Eichler(1979). It provides us the evidence of the cosmic ray acceleration in the shock wave.

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