Nonuniform magnetohydrodynamic nature of the solar corona. I. Basic solutions

Journal Article · Wed Jun 01 00:00:00 EDT 1988 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/166445· OSTI ID:6920791

Priest, E R

The highly structured nature of the corona is explained in terms of standing MHD disturbances of several types which are spread over extended regions rather than being concentrated in narrow regions like shock waves. The results suggest that plumes of enhanced plasma pressure and flow may be associated with fast-mode compressions having streamlines and magnetic field lines than converge relative to a uniform background corona. The deflection and compression of a coronal ray and the legs of a mass ejection may also be the result of a fast-mode compression. Holes or voids of reduced plasma and flow may be created by slow-mode compressions. 22 references.

• Research Organization: High Altitude Observatory, Boulder, CO (USA)
• OSTI ID: 6920791
• Journal Information: Astrophys. J.; (United States), Vol. 329
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
SOLAR CORONA
MAGNETOHYDRODYNAMICS
COMPRESSION
INHOMOGENEOUS PLASMA
MAGNETIC FIELDS
MASS TRANSFER
SHOCK WAVES
ATMOSPHERES
FLUID MECHANICS
HYDRODYNAMICS
MECHANICS
PLASMA
STELLAR ATMOSPHERES
STELLAR CORONAE
640104* - Astrophysics & Cosmology- Solar Phenomena