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Pre-Eruption Magnetic Configurations in the Active-Region Solar Photosphere

Published online by Cambridge University Press:  26 August 2011

Manolis K. Georgoulis
Manolis K. Georgoulis*
Affiliation:
Research Center for Astronomy and Applied Mathematics (RCAAM), Academy of Athens, 4 Soranou Efesiou Street, Athens, Greece, GR-11527 email: manolis.georgoulis@academyofathens.gr
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Abstract

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Most solar eruptions occur above strong photospheric magnetic polarity inversion lines (PILs). What overlays a PIL is unknown, however, and this has led to a debate over the existence of sheared magnetic arcades vs. helical magnetic flux ropes. We argue that this debate may be of little meaning: numerous small-scale magnetic reconnections, constantly triggered in the PIL area, can lead to effective transformation of mutual to self magnetic helicity (i.e. twist and writhe) that, ultimately, may force the magnetic structure above PILs to erupt to be relieved from its excess helicity. This is preliminary report of work currently in progress.

Keywords

Sun: coronal mass ejections (CMEs)Sun: flaresSun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 495 - 498
Copyright
Copyright © International Astronomical Union 2011

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