Solar Magnetoconvection
Abstract
The structure and dynamics of pores and sunspots have defied simple theoretical descriptions. Over the past century, and particularly the past few decades, two competing and somewhat disjoint models have developed. One envisions sunspots to be the surface manifestation of a set of magnetic flux tubes, which form a distinct set, separate from the surrounding field-free plasma. The other again has them consisting of a single large flux concentration, which exists within a continuum of plasma and magnetic fields and in which normal fluid dynamical processes occur. Here I review recent progress in explaining the structure and dynamics of sunspots based upon the latter model. Several series of highly idealized numerical simulations suggest that this model can indeed explain a large number of the fundamental behaviors observed in sunspots including heating of the umbra, umbral dots, penumbra grains, the Evershed effect, "fluted" and "spined" penumbra, the formation of penumbra and sunspot moats and the formation of X-ray anemonae.
- Publication:
-
SOHO-9 Workshop on Helioseismic Diagnostics of Solar Convection and Activity
- Pub Date:
- 1999
- Bibcode:
- 1999soho....9E...7H