Induced mass and wave motions in the lower solar atmosphere. I. Effects of shear motion of flux tubes

Journal Article · Tue Mar 15 00:00:00 EST 1983 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160834· OSTI ID:5774119

Wu, S T; Hu, Y Q; Nakagawa, Y; Tandberg-Hanssen, E

Mass and wave motions induced in the solar atmosphere by differential movements of the photospheric footpoints of magnetic flux have been examined as an initial boundary-value problem for two-dimensional, time dependent, nonplanar, ideal (i.e., nondissipative) MHD flow. Numerical solutions have been obtained by a newly developed full implicit continuous eulerian (FICE) scheme. For convenience, the initial solar atmosphere was assumed isothermal (approx.10/sup 5/ K) and in hydrostatic equilibrium, and the initial configuration of the magnetic field was chosen to be a dipole configuration. The numerical results show that: (1) in the continuous total energy buildup in the solar atmosphere due to the shear motions of the footpoints, the rate of magnetic energy buildup is 4 times faster than the rate of the other modes (potential, thermal, and kinetic energy) for shear velocities less than 20 km s/sup -1/; (2) the velocity of vertical mass motions is of the order of approx.10 km s/sup -1/; (3) the mass and wave motions are controlled by the form and magnitude of the movements of the footpoints and by the initial value of the plasma.

• Research Organization: The University of Alabama in Huntsville
• OSTI ID: 5774119
• Journal Information: Astrophys. J.; (United States), Vol. 266:2
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
SOLAR ATMOSPHERE
MAGNETOHYDRODYNAMICS
BOUNDARY CONDITIONS
BOUNDARY-VALUE PROBLEMS
FLUID FLOW
MAGNETIC FIELD CONFIGURATIONS
MAGNETIC FIELDS
MAGNETIC FLUX
NUMERICAL SOLUTION
PLASMA
SHEAR
STAR MODELS
ATMOSPHERES
FLUID MECHANICS
HYDRODYNAMICS
MATHEMATICAL MODELS
MECHANICS
640104* - Astrophysics & Cosmology- Solar Phenomena