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Solar Magnetoconvection

Published online by Cambridge University Press:  08 February 2017

Å. Nordlund  and
R. F. Stein
Å. Nordlund
Affiliation:
Copenhagen University Observatory ⊘ster Voldgade 3 1350 Copenhagen K Denmark
R. F. Stein
Affiliation:
Dept. of Physics and Astronomy Michigan State University, East Lansing, MI 48823 U.S.A.

Abstract

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As a prelude to discussing the interaction of magnetic fields with convection, we first review some general properties of convection in a stratified medium. Granulation, which is the surface manifestation of the major energy carrying convection scales, is a shallow phenomenon. Below the surface, the topology changes to one of filamentary cool downdrafts, immersed in a gently ascending isentropic background. The granular downflows merge into more widely separated downdrafts, on scales of mesogranulation and super-granulation.

The local topology and time evolution of the small scale, kilo Gauss, network and facular magnetic field elements are controlled by convection on the scale of granulation. The topology and time evolution of larger scale magnetic field concentrations are controlled by the hierarchical structure of the horizontal components of the large scale velocity field. In sunspots, the small scale magnetic field structure determines the energy balance, the systematic flows and the waves. Below the surface, the small scale structure of the magnetic field may change drastically, with little observable effect at the surface. We discuss results of some recent numerical simulations of sunspot magnetic fields, and some mechanisms that may be relevant in determining the topology of the sub-surface magnetic field. Finally, we discuss the role of active region magnetic fields in the global solar dynamo.

Type
IV. Magnetohydrodynamics of the Photosphere
Information
Symposium - International Astronomical Union , Volume 138: Solar Photosphere: Structure, Convection and Magnetic Fields , 1990 , pp. 191 - 211
Copyright
Copyright © Kluwer 1990 

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