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Flux emergence and interaction with a coronal field: 3D MHD simulations

Published online by Cambridge University Press:  01 November 2006

V. Archontis ,
F. Moreno-Insertis ,
K. Galsgaard  and
A. W. Hood
V. Archontis
Affiliation:
School of Mathematics and Statistics, University of St.Andrews, North Haugh, Fife KY16 9SS, UK email: vasilis@mcs.st-and.ac.uk, alan@mcs.st-and.ac.uk
F. Moreno-Insertis
Affiliation:
Instituto de Astrofisica de Canarias, Via Lactea s/n, 38200 La Laguna, Spain email: fmi@ll.iac.es
K. Galsgaard
Affiliation:
Niels Bohr Institute, Juliane Maries Vej 30, 2100 Copenhagen, Denmark email: kg@astro.ku.dk
A. W. Hood
Affiliation:
School of Mathematics and Statistics, University of St.Andrews, North Haugh, Fife KY16 9SS, UK email: vasilis@mcs.st-and.ac.uk, alan@mcs.st-and.ac.uk
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Abstract

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The dynamic process of magnetic flux emergence from the solar interior to the outer atmosphere may well be related with eruptive phenomena and intense events of the Solar activity. However, the physics of the emergence is not still well understood. Thus, we have performed 3D MHD simulations to study the rising motion of a twisted flux tube from the convection zone of the Sun and its interaction with a preexisting coronal magnetic field. The results show that the reconnection process depends criticaly on the initial relative orientation between the two magnetic flux systems into contact. On the other hand, the overal process of emergence depends mostly on the dynamics of the sub-photospheric plasma.

Keywords

MHDmagnetic fieldscorona
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 53 - 56
Copyright
© 2006 International Astronomical Union