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The Evolution of Photospheric Source Regions of CMEs

Published online by Cambridge University Press:  03 June 2005

K. Muglach  and
K. Dere
K. Muglach
Affiliation:
Artep, Inc., Naval Research Laboratory, Washington, DC, USA email: muglach@nrl.navy.mil
K. Dere
Affiliation:
George Mason University, Fairfax, VA, USA email:kdere@gmu.edu
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Abstract

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In this presentation we determine the source regions of CMEs that were observed with SoHO/LASCO during times of solar activity maximum (Feb./Mar. 2000) and during the declining phase of the solar cycle (Nov./Dec. 2002). The CMEs were traced back onto the disk and EIT EUV images were used for identifying the sources. With the help of MDI synoptic magnetograms we follow the evolution of the photospheric magnetic flux about 24h before and 12h after the event. We find that about 87% of the identified CME source regions show small–scale flux changes before the event, usually flux emergence and/or flux disappearance. In 13% of the cases we find no signature of photospheric flux changes.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Sun: magnetic fieldsSun: photosphereSun: coronal mass ejections (CMEs)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS226 , September 2004 , pp. 179 - 183
Copyright
© 2005 International Astronomical Union