Volume 514, May 2010
|Number of page(s)||4|
|Published online||19 May 2010|
Flux emergence and coronal eruption
School of Mathematics and Statistics, University of St. Andrews, North Haugh,
St. Andrews, Fife, KY16 9SS, UK e-mail: [vasilis;alan]@mcs.st-and.ac.uk
Accepted: 5 February 2010
Aims. Our aim is to study the photospheric flux distribution of a twisted flux tube that emerges from the solar interior. We also report on the eruption of a new flux rope when the emerging tube rises into a pre-existing magnetic field in the corona.
Methods. To study the evolution, we use 3D numerical simulations by solving the time-dependent and resistive MHD equations. We qualitatively compare our numerical results with MDI magnetograms of emerging flux at the solar surface.
Results. We find that the photospheric magnetic flux distribution consists of two regions of opposite polarities and elongated magnetic tails on the two sides of the polarity inversion line (PIL), depending on the azimuthal nature of the emerging field lines and the initial field strength of the rising tube. Their shape is progressively deformed due to plasma motions towards the PIL. Our results are in qualitative agreement with observational studies of magnetic flux emergence in active regions (ARs). Moreover, if the initial twist of the emerging tube is small, the photospheric magnetic field develops an undulating shape and does not possess tails. In all cases, we find that a new flux rope is formed above the original axis of the emerging tube that may erupt into the corona, depending on the strength of the ambient field.
Key words: magnetohydrodynamics (MHD) / Sun: activity / Sun: corona / magnetic fields
© ESO, 2010
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