Mathematics
Scientific paper
Sep 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986phdt.........5k&link_type=abstract
Ph.D. Thesis Arizona Univ., Tucson.
Mathematics
1
Astronomical Models, Boundary Value Problems, Galactic Cosmic Rays, Hydrodynamics, Pressure Gradients, Shock Waves, Stellar Winds, Acceleration (Physics), Boundary Conditions, Iterative Solution, Singularity (Mathematics), Transonic Flow
Scientific paper
A two-fluid hydrodynamical model describing the modification of a stellar wind flow due to its interaction with galactic cosmic-rays is investigated. The two fluids consist of the thermal stellar wind gas and the galactic cosmic-rays. A polytropic one fluid model is used to describe the stellar wind gas, and the cosmic rays modify the wind via their pressure gradient. The equations used are essentially those employed in two fluid hydrodynamical models of cosmic-ray shock acceleration by the first order Fermi mechanism, but suitably modified to apply in a spherical geometry and including the effects of gravity on the flow. The model shows the deceleration of the wind upstream of the shock by the positive galactic cosmic-ray pressure gradient. The fluid polytropic stellar winds are discussed and how to insert shock in the flow. A description of the singularities of the equations is also presented. The system of equations is first solved by a finite difference method in the test particle approximation with appropriate boundary conditions applied at infinity, at the wind termination shock, and at the star. A perturbation scheme to determine the modification of the wind by the cosmic rays is then developed. Finally a numerical iteration is employed to exactly solve the equations.
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