Magnetic field propagation in a stellar dynamo

Journal Article · Sat Jun 01 04:00:00 EDT 1985 · J. Stat. Phys.; (United States)

DOI:https://doi.org/10.1007/BF01008347· OSTI ID:5308478

Glatzmaier, G A

Numerical simulations of stellar dynamos are reviewed. Dynamic dynamo models solve the nonlinear, three-dimensional, time-dependent, magnetohydrodynamic equations for the convective velocity, the thermodynamic variables, and the generated magnetic field in a rotating, spherical shell of ionized gas. When the dynamo operates in the convection zone, the simulated magnetic fields propagate away from the equator in the opposite direction inferred from the solar butterfly diagram. When simulated at the base of the convection zone, the fields propagate in the right direction at roughly the right speed. However, owing to the numerical difficulty, a full magnetic cycle has not been simulated in this region. As a result, it is still uncertain where and how the solar dynamo operates.

• Research Organization: Theoretical Divisio, Los Alamos National Laboratory, Los Alamos, New Mexico
• OSTI ID: 5308478
• Journal Information: J. Stat. Phys.; (United States), Journal Name: J. Stat. Phys.; (United States) Vol. 39:3; ISSN JSTPB
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
640104 -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
CONVECTION
ENERGY TRANSFER
FLUID MECHANICS
HEAT TRANSFER
HYDRODYNAMICS
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MAIN SEQUENCE STARS
MASS TRANSFER
MECHANICS
NONLINEAR PROBLEMS
SIMULATION
SOLAR ACTIVITY
STARS
SUN
THREE-DIMENSIONAL CALCULATIONS