Solar Supergranulation.
Abstract
A convective process originating some 10,000 km below the solar surface was studied. Several observations designed to study the process are examined. An alternate approach taken in understanding stellar convection was the study of the dMe stars. A discussion of observational results within the framework of solar and stellar convection zone-magnetic interactions is provided. Simultaneous velocity, magnetic field, and chromospheric emission network data were used to study the lifetimes, the vertical velocity flow, and the transport of magnetic fields associated with supergranulation. Horizontal magnetic field motions take two forms: (1) an apparent slow breakup of existing flux points; and (2) a rapid motion of flux following the emergence of new magnetic field. The latter may be associated with the formation of a new supergranule. Results are consistent with a generalized stellar model in which strong magnetic fields are shown to be generated deep within the star.
- Publication:
-
Ph.D. Thesis
- Pub Date:
- 1975
- Bibcode:
- 1975PhDT.........2W
- Keywords:
-
- Physics: Astronomy and Astrophysics;
- Convection Currents;
- Convective Flow;
- Solar Atmosphere;
- Solar Activity Effects;
- Solar Magnetic Field;
- Solar Physics;
- Solar Physics