Volume 492, Number 2, December III 2008
|Page(s)||L35 - L38|
|Published online||20 November 2008|
Letter to the Editor
Eruption of magnetic flux ropes during flux emergence
School of Mathematics and Statistics, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK e-mail: email@example.com
2 LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France e-mail: firstname.lastname@example.org
Accepted: 5 November 2008
Aims. We investigate the formation of flux ropes in a flux emergence region and their rise into the outer atmosphere of the Sun.
Methods. We perform 3D numerical experiments by solving the time-dependent and resistive MHD equations.
Results. A sub-photospheric twisted flux tube rises from the solar interior and expands into the corona. A flux rope is formed within the expanding field, due to shearing and reconnection of field lines at low atmospheric heights. If the tube emerges into a non-magnetized atmosphere, the flux rope rises, but remains confined inside the expanding magnetized volume. In contrast, if the expanding tube is allowed to reconnect with a pre-existing coronal field, the flux rope experiences a full eruption with a rise profile that is in qualitative agreement with erupting filaments and Coronal Mass Ejections.
Key words: magnetohydrodynamics (MHD) / methods: numerical / Sun: activity / Sun: corona / Sun: magnetic fields
© ESO, 2008
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.