Statistics – Computation
Scientific paper
Jun 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...329.1009p&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 329, June 15, 1988, p. 1009-1022.
Statistics
Computation
4
Computational Astrophysics, Magnetohydrodynamic Stability, Nonuniform Plasmas, Shock Waves, Solar Corona, Continuity Equation, Ohms Law, Polytropic Processes
Scientific paper
The highly structured nature of the solar corona is created largely by the magnetic field, and the author shows how such structure can be understood in terms of standing MHD disturbances of several types, spread over extended regions rather than being concentrated in narrow regions like shock waves. They can be compressions, in which the plasma pressure increases, or expansions in which it decreases. The compressions can be of fast-mode type if the magnetic field increases or of slow-mode type when it decreases, and vice-versa for the expansions. A general method is developed for describing these structures, and it is applied in simple examples to coronal plumes (fast-mode compressions), coronal holes or depletions (slow-mode compressions), the deflection of coronal rays (fast-mode compressions), and the legs of coronal mass ejections (fast-mode compressions).
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