Magnetic structures of active regions and their link to coronal mass ejections

Details Magnetic structures of active regions and their link to coronal mass ejections Magnetic structures of active regions and their link to coronal mass ejections

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh51c..03y&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH51C-03

Physics

2134 Interplanetary Magnetic Fields, 2169 Sources Of The Solar Wind, 2722 Forecasting, 7513 Coronal Mass Ejections, 7524 Magnetic Fields

Scientific paper

olar coronal mass ejections (CMEs) are a principal link that connects the chain of events in the solar atmosphere, interplanetary space and the earth's magnetic environment. The central objective of our study is to advance our understanding of physical processes in CMEs and related phenomena, including their ultimate origin, precursors and near sun evolution as well as their link to the interplanetary phenomena. Earlier studies unanimously suggest that there is a straightforward relationship between the magnetic fields of erupted filaments and magnetic clouds at 1AU. However, the situation is more complicated and less understood in the case of eruptions from solar active regions. We combined photospheric magnetograms, chromospheric and coronal images as well as solar wind data of high spatial and temporal resolution in order to i) determine the basic characteristics of the initial pre-eruption magnetic configuration in an active region and ii) find a link between these characteristics and the magnetic fields in interplanetary CMEs (ICMEs) at 1AU. Our results show a good correspondence between the directions of the helical magnetic fields in interplanetary ejecta and in the source active regions. We will also demonstrate how the combination of the solar surface and solar wind data may be used to discriminate between different CME models and to predict the sign of the interplanetary magnetic field at 1AU.

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