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Field Strength Vs. Temperature Relation and the Structure of Sunspots

Published online by Cambridge University Press:  12 April 2016

S.K. Solanki ,
U. Walther  and
W. Livingston
S.K. Solanki
Affiliation:
Institute of Astronomy, ETH-Zentrum, CH-8092 Zürich, Switzerland
U. Walther
Affiliation:
Institute of Astronomy, ETH-Zentrum, CH-8092 Zürich, Switzerland
W. Livingston
Affiliation:
National Solar Observatory, NOAO, *, P.O.Box 26732, Tucson AZ 85726, USA

Abstract

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The relationship between the magnetic vector and the temperature of a large symmetric sunspot is studied on the basis of 1.56 µm spectra. From this relation we estimate the shape of the τ = 1 surface. i.e. the Wilson depression, as a function of radial distance in the sunspot. We find that the Wilson depression is relatively small throughout the penumbra and changes by 200–500 km at the umbral boundary. We also estimate the magnitude of magnetic gradients and curvature forces.

Keywords

Solar Magnetic FieldsSunspotsMHD
Type
Session 1. Structure of Active Regions
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 48 - 51
Copyright
Copyright © Astronomical Society of the Pacific 1993

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