Other
Scientific paper
Sep 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..95..291s&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 95, no. 2, Sept. 1983, p. 291-298
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1
Interplanetary Magnetic Fields, Magnetohydrodynamic Flow, Shock Wave Propagation, Solar Flares, Solar Wind, Ideal Gas, Isothermal Flow, Shock Fronts, Spherical Waves
Scientific paper
An analytical solution is obtained for self-similar flow behind a strong spherical shock wave in the presence of a magnetic field. Use is made of the method proposed by Laumbach and Probstein (1969). Here, the total energy of the flow between the shock and piston is dependent on the shock radius obeying a power law. The shock is propagating into a perfect gas that is at rest with nonuniform density and magnetic field. The same method is then used to reinvestigate the problem of Ranga Rao and Ramana (1973) in a nonuniform atmosphere for isothermal flow. The radiation propagates radially with a constant power input which is absorbed completely in the shock layer of a spherically expanding shock wave. The gas here is optically thin and thick ahead and behind the shock front, respectively, and the flow is particle isentropic behind the shock wave.
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