Chapter

Magnetism and convection

Leon Mestel

in Stellar Magnetism

Published in print February 2012 | ISBN: 9780199641741
Published online May 2012 | e-ISBN: 9780191738609 | DOI: http://dx.doi.org/10.1093/acprof:oso/9780199641741.003.0004

Series: International Series of Monographs on Physics

                   Magnetism and convection

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Our Sun is a veritable laboratory for the study of magnetohydrodynamics. It exhibits a wide variety of phenomena — sunspots, flares, prominences — in which a magnetic field is clearly the crucial feature. Furthermore, late-type stars such as the Sun spontaneously develop a sub-photospheric convective zone, with motions observable most strikingly as the violent, small-scale granulation, as well as the larger-scale mesoand supergranulation. This chapter is concerned primarily with some aspects of the interaction between turbulent convection and a magnetic field in the Sun, and so also in other late-type stars with their deep outer convection zones. Topics discussed include the angular velocity distribution in a convective zone; the effect of convective motions on an imposed magnetic field; a strong imposed field and the onset of convection; developments in non-linear theory; sunspots, pores, and isolated flux tubes; magnetic buoyancy; and solar activity.

Keywords: magnetohydrodynamics; turbulent convection; magnetic field; Sun; late-type stars; convective zones; angular velocity; sunspots; flares

Chapter.  23762 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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