Numerical simulations of convectively excited gravity waves
Conference
·
OSTI ID:5705615
Magneto-convection and gravity waves are numerically simulated with a nonlinear, three-dimensional, time-dependent model of a stratified, rotating, spherical fluid shell heated from below. A Solar-like reference state is specified while global velocity, magnetic field, and thermodynamic perturbations are computed from the anelastic magnetohydrodynamic equations. Convective overshooting from the upper (superadiabatic) part of the shell excites gravity waves in the lower (subadiabatic) part. Due to differential rotation and Coriolis forces, convective cell patterns propagate eastward with a latitudinally dependent phase velocity. The structure of the excited wave motions in the stable region is more time-dependent than that of the convective motions above. The magnetic field tends to be concentrated over giant-cell downdrafts in the convective zone but is affected very little by the wave motion in the stable region.
- Research Organization:
- Los Alamos National Lab., NM (USA)
- DOE Contract Number:
- W-7405-ENG-36
- OSTI ID:
- 5705615
- Report Number(s):
- LA-UR-83-2896; CONF-8308136-1; ON: DE84001867
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
CONVECTION
GRAVITY WAVES
MATHEMATICAL MODELS
MOTION
NUMERICAL SOLUTION
PHASE VELOCITY
ROTATION
SIMULATION
STAR MODELS
STELLAR ATMOSPHERES
VELOCITY
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
CONVECTION
GRAVITY WAVES
MATHEMATICAL MODELS
MOTION
NUMERICAL SOLUTION
PHASE VELOCITY
ROTATION
SIMULATION
STAR MODELS
STELLAR ATMOSPHERES
VELOCITY