Theories of sunspot structure and evolution
Abstract
Various attempts to model all or part of the known phenomena associated with sunspots are reviewed. In summary, sunspots appear and grow as groups within active regions. Simple prototypes are the leader L and follower F spots, with the F spots decaying within a week, like a group, while L spots first form a moat-like structure and then last for several solar rotations. The magnetic structure stability of a sunspot is discussed, together with the reasons for the relative coolness, i.e., 3500-4000 K. A necessity is mentioned for understanding the subsurface structure of the spots, although the phenomena may in fact be shallow. Attention is given to the features and deficiencies of three sunspot models. It is suggested that improvements in modeling may be obtained from studies of the irradiance variability data, the growth and decay rates, time-dependent studies of the simultaneous magnetic and velocity fields and brightness patterns in the region around sunspots, and observations by the solar orbiting telescope of the ultrafine structure of the umbrae and penumbrae.
- Publication:
-
The Physics of Sunspots
- Pub Date:
- 1981
- Bibcode:
- 1981phss.conf...83W
- Keywords:
-
- Sunspots;
- Convective Heat Transfer;
- Cooling;
- Energy Transfer;
- Evolution (Development);
- Magnetic Fields;
- Solar Physics