Physics
Scientific paper
Mar 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980soph...65..369p&link_type=abstract
Solar Physics, vol. 65, Mar. 1980, p. 369-385.
Physics
42
Magnetohydrodynamic Stability, Solar Corona, Solar Prominences, Solar Wind, Transient Response, Gas Pressure, Magnetic Field Configurations, Mathematical Models, Plasma Equilibrium, Solar Flares, Solar Flux, Solar Magnetic Field, Solar X-Rays
Scientific paper
The proposed semiquantitative MHD model incorporates a cause and effect relationship between coronal transients and eruptive prominences. The model assumes an MHD mechanism in which the magnetic field of the filament and beneath it provides an outward pressure gradient across the helmet above. If this field conserves its flux as it rises, then this magnetic force per unit mass falls off with distance as the inverse square of the displacement. Since the restoring magnetic tension and gravity forces in the overlying field decrease with distance at the same rate, the ratio of total outward to inward force is independent of the radial distance from the sun. This situation is shown to be one of neutral stability. A mathematical formulation of the mechanism yields a solution in which the velocity increases sharply close to the sun but quickly approaches a constant value. The width increases linearly with radial distance.
No associations
LandOfFree
Eruptive prominences and coronal transients does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Eruptive prominences and coronal transients, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Eruptive prominences and coronal transients will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1575570