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The Small-Scale Photospheric Magnetic Field as an Indicator of the Dynamo

Published online by Cambridge University Press:  12 April 2016

K. Petrovay  and
G. Szakály
K. Petrovay
Affiliation:
Eötvös University, Department of Astronomy, Budapest, Ludovika tér 2, H-1083Hungary
G. Szakály
Affiliation:
Eötvös University, Department of Astronomy, Budapest, Ludovika tér 2, H-1083Hungary

Abstract

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The presently widely accepted view that the solar dynamo operates near the base of the convective zone makes it difficult to relate the magnetic fields observed in the solar atmosphere to the fields in the dynamo layer. The large amount of observational data concerning photospheric magnetic fields could in principle be used to impose constraints on dynamo theory, but in order to infer these constraints the above mentioned “missing link” between the dynamo and surface fields should be found. This paper proposes such a link by modeling the passive vertical transport of thin magnetic flux tubes through the convective zone.

Type
Session 2. Theory of Active Region Structure
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 143 - 146
Copyright
Copyright © Astronomical Society of the Pacific 1993

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