Equatorial propagation of axisymmetric magnetogasdynamic shocks with increasing energy. I

Details Equatorial propagation of axisymmetric magnetogasdynamic shocks with increasing energy. I Equatorial propagation of axisymmetric magnetogasdynamic shocks with increasing energy. I

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..92..191s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 92, no. 1, May 1983, p. 191-195.

Astronomy and Astrophysics

Astrophysics

2

Equatorial Atmosphere, Magnetohydrodynamic Waves, Shock Wave Propagation, Solar Magnetic Field, Equations Of Motion, Mathematical Models, Numerical Integration

Scientific paper

Consideration is given to a model in which the magnetic field distribution is proportional to 1/r; the total energy is of an increasing order and it never becomes constant. The solutions correspond to a blast wave produced by intense prolonged solar flare activity in a case where the wave is driven by fresh erupting solar plasma for some time and has energy that tends to increase with time as it propagates away from the sun. It is assumed that the shock advances into a conducting gas of spatially decreasing density and is pervaded by a spatially decreasing magnetic field. The atmosphere is taken to be initially at rest and cold, that is, at zero temperature and pressure. The body forces from the earth's gravitational and wind effects are neglected.

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