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Sunspots and magnetohydrodynamic flows

Published online by Cambridge University Press:  14 August 2015

G. F. Anderson  and
D. H. Menzel
G. F. Anderson
Affiliation:
Harvard College Observatory, Cambridge, Mass., U.S.A.
D. H. Menzel
Affiliation:
Harvard College Observatory, Cambridge, Mass., U.S.A.

Abstract

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Theoretical techniques are developed to study compressible, steady-state, magnetically aligned gas flows in sunspot regions. The flows are adiabatic and occur in a known streamline configuration. The non-linear parabolic partial differential equation describing the flow reduces to an ordinary linear differential equation. The solutions are briefly discussed.

Type
Part II: Theoretical Aspects
Information
Symposium - International Astronomical Union , Volume 35: Structure and Development of Solar Active Regions , 1968 , pp. 142 - 147
Copyright
Copyright © Reidel 1968 

References

Koshlyakov, N.S., Smirnov, M.M., Gliner, E.B. (1964) Differential Equations of Mathematical Physics, North-Holland Publ. Co., Amsterdam.Google Scholar
Menzel, D.H., Shore, B.W. (1966) ‘Sunspots, Magnetic Fields and the Structure of the Solar Atmosphere’, in Atti del Convegno sulle macchie solari, IV. Centenario della Nascità di Galileo Galilei, Ed. by Barbera, G., Florence, p. 226.Google Scholar