Magnetohydrodynamics of atmospheric transients. II - Two-dimensional numerical results for a model solar corona

Details Magnetohydrodynamics of atmospheric transients. II - Two-dimensional numerical results for a model solar corona Magnetohydrodynamics of atmospheric transients. II - Two-dimensional numerical results for a model solar corona

Jan 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...219..324w&link_type=abstract

Astrophysical Journal, Part 1, vol. 219, Jan. 1, 1978, p. 324-335.

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53

Magnetic Field Configurations, Magnetohydrodynamic Waves, Shock Waves, Solar Corona, Solar Magnetic Field, Surges, Dynamic Response, Plasma Interactions

Scientific paper

A systematic study of dynamic response of the inner solar corona is made within the context of two-dimensional, time-dependent plane hydromagnetics. The governing equations are written in r-phi coordinates (i.e., in the solar equatorial plane), and numerical solutions are obtained by introducing an impulsive temperature enhancement within a rectangular region (i.e., 'box') in an initially isothermal corona in magnetohydrostatic equilibrium. Effects of the magnetic field configuration are illustrated for initially open (radial) and closed (azimuthal) magnetic fields by comparison with the nonmagnetic response. The channeling or blocking effects by the magnetic fields on the mass motion of solar plasma as the consequence of the evolution of fast and slow mode MHD shock waves are demonstrated. Some physically significant applications of the results, useful for the interpretation of observations, are discussed. It is noted, for example, that coronal transients observed in white light probably occur within essentially radial field topologies.

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