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Evolution of Large and Small Scale Magnetic Fields in the Sun

Published online by Cambridge University Press:  12 April 2016

Peter A. Fox ,
Michael L. Theobald  and
Sabatino Sofia
Peter A. Fox
Affiliation:
Center for Solar and Space Research, Yale University, P.O. Box 6666, New Haven, CT 06511USA
Michael L. Theobald
Affiliation:
Center for Solar and Space Research, Yale University, P.O. Box 6666, New Haven, CT 06511USA
Sabatino Sofia
Affiliation:
Center for Solar and Space Research, Yale University, P.O. Box 6666, New Haven, CT 06511USA

Abstract

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This paper will discuss issues relating to the detailed numerical simulation of solar magnetic fields, those on the small scale which are directly observable on the surface, and those on larger scales whose properties must be deduced indirectly from phenomena such as the sunspot cycle. Results of simulations using the ADISM technique will be presented to demonstrate the importance of the treatment of Alfvén waves, the boundary conditions, and the statistical evolution of small scale convection with magnetic fields. To study the large scale fields and their time dependence, the magnetic resistivity plays an important role; its use will be discussed in the paper.

Type
Part III Solar magnetism and large-scale flows
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 218 - 222
Copyright
Copyright © Springer-Verlag 1991

References

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