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Magnetic Flux Transport and Formation of Filament Channels

Published online by Cambridge University Press:  12 April 2016

A.A. van Ballegooijen ,
N.P. Cartledge  and
E.R. Priest
A.A. van Ballegooijen
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
N.P. Cartledge
Affiliation:
Mathematical and Computational Sciences Department, University of St. Andrews, KY16 9SS Scotland, UK
E.R. Priest
Affiliation:
Mathematical and Computational Sciences Department, University of St. Andrews, KY16 9SS Scotland, UK

Abstract

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We present a model of the transport of photospheric and coronal magnetic fields with the aim of explaining the observed global pattern of dextral and sinistral filaments on the quiet sun. The model is based on the assumption that the axial field in a filament channel originates in the surrounding coronal arcade. The model predicts that switchbacks in the polarity inversion line have opposite chirality on the two arms of the switchback: the higher latitude “lead” arm has sinistral (dextral) orientation in the North (South), while the lower latitude “return” arm has dextral (sinistral) orientation. This is in conflict with prominence observations which show that the chirality is the same on the two arms of a switchback. The model predicts the wrong sign of the axial field in polar crown filaments. This suggests that axial field in quiescent filaments are not produced by differential rotation acting on the surrounding coronal arcades.

Type
Birth and Death of Filaments
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 265 - 268
Copyright
Copyright © Astronomical Society of the Pacific 1998

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