Model for quiescent solar prominences

Journal Article · Wed Aug 15 04:00:00 EDT 1979 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/157290· OSTI ID:5894562

Milne, A M; Priest, E R; Roberts, B

A one-dimensional model is computed for a quiescent prominence in both magnetohydrostatic equilibrium (under a balance between gravity, pressure gradients, and the J x B force) and thermal equilibrium (under a balance between thermal conduction, radiation, and wave heating). Prominence widths comparable to those observed can be obtained for some forms of the energy balance terms.The effects of changing the coronal plasma pressure p/sub 1/, the horizontal magnetic field strength B/sub x/, and the inclination Phi of the horizontal magnetic field to the prominence normal are investigated. It is found that an equilibrium state is impossible when either the plasma beta (..beta..equivalent2..mu..p/sub 1//B/sub x//sup 2/) or the magnetic field shear (Phi) is too high. The limit on the plasma ..beta.. leads to a minimum possible height for prominence formation and implies that active-region prominences can form lower in the atmosphere than quiescent ones. It also gives a reason for the existence of ''feet'' in quiescent prominences. Exceeding the maximum shear may explain the eruption of a prominence.

• Research Organization: Department of Applied Mathematics, University of St. Andrews, Fife, Scotland
• OSTI ID: 5894562
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 232:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BOUNDARY CONDITIONS
ENERGY BALANCE
ENERGY TRANSFER
FLUID MECHANICS
HEAT TRANSFER
HYDRODYNAMICS
MAGNETIC FIELD CONFIGURATIONS
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MATHEMATICAL MODELS
MECHANICS
PLASMA
SOLAR ACTIVITY
SOLAR CORONA
SOLAR PROMINENCES
STAR MODELS
THERMAL CONDUCTION