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Formation of Arching Flux Tubes at the Base of the Solar Convection Zone

Published online by Cambridge University Press:  13 May 2016

Y. Fan
Y. Fan*
Affiliation:
High Altitude Obs., National Center for Atmospheric Research, 3450 Mitchell Lane, Boulder, CO 80301, USA

Abstract

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Solar active regions are believed to correspond to the topmost portions of Ω-shaped arching flux tubes that have risen buoyantly from the base of the solar convection zone, where strong toroidal magnetic fields are being generated by the dynamo process. The development of such emerging Ω-loops is likely a result of the buoyant instability associated with the submerged toroidal magnetic field. Using an anelastic MHD code, we simulate the formation of buoyant, arching flux tube structures as a result of the non-linear growth of the undular instability of a neutrally buoyant layer of horizontal, unidirectional magnetic field at the base of the solar convection zone.

Type
Session III: Active Region Structure and Dynamics
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 273 - 275
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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