Journal of Emerging Trends in Engineering and Applied Sciences: Research Areas

Abstract:
Using a framework of the radiation approximation followed by a two-term perturbation expansion for cosmic ray transport in the spherical polar coordinates (r, , &, o) we identify the effect of cosmic ray radiation on shock dominated transport. The theory gives the possibility of an approximate description of some parameters (radiation and temperature) in cosmic ray propagation. This can be applied to solar wind acceleration. When the buoyancy parameter Fr is negligible, we find that the cosmic ray density at shock boundary (En) decreases with increasing temperature. It is also observed that the variation of radiation parameter N in cosmic ray transport has no significant effect in the temperature distribution. Thus, even when radiation is significant, it does not really modify the temperature within the cosmic ray region. However, for increases in the density at shock boundaries say (En), the temperature distribution decreases.

Keywords: cosmic rays, background plasma, radiative shocks, pressure tensor, fluid formalism.

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