The nonuniform magnetohydrodynamic nature of the solar corona. III - Cylindrical geometry

Details The nonuniform magnetohydrodynamic nature of the solar corona. III - Cylindrical geometry The nonuniform magnetohydrodynamic nature of the solar corona. III - Cylindrical geometry

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347.1167d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 15, 1989, p. 1167-1175. Research supported by SERC.

Physics

2

Coronal Holes, Cylindrical Plasmas, Magnetic Field Configurations, Magnetohydrodynamic Stability, Solar Corona, Solar Magnetic Field, Equations Of Motion, Plasma Density, Plasma Pressure, Solar Atmosphere

Scientific paper

The method developed by Priest in 1988 for modeling steady MHD disturbances in the solar corona is extended to a cylindrical geometry, which is more realistic for three-dimensional structures, such as plumes and coronal holes, which are observed in the corona. Both axial symmetric and nonaxial magnetic fields are treated. The basic characteristics of the axisymmetric solutions are found to be similar to the previous Cartesian case. Quantitatively, the interactions are stronger in the central region and weaker at the outer boundary. Pressure gradients are also found to be smaller. Solutions dependent on all three spatial variables exhibit an asymmetry because of the angular dependence. They depend upon the azimuthal magnetic field imposed at the coronal base. The solutions found in this paper may be useful in interpreting the physics of MHD interactions observed in numerical experiments and also in the solar atmosphere.

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