Properties of Magnetic Clouds Resulting from Eruption of Coronal Sigmoids

Details Properties of Magnetic Clouds Resulting from Eruption of Coronal Sigmoids Properties of Magnetic Clouds Resulting from Eruption of Coronal Sigmoids

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh31c08l&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH31C-08

Physics

7509 Corona, 7513 Coronal Mass Ejections, 7536 Solar Activity Cycle (2162)

Scientific paper

We study over 40 eruptions which originated with coronal sigmoids seen in Yohkoh SXT images, with subsequently observed in situ magnetic clouds (MCs) and geomagnetic storms at 1~AU. We correlate solar and interplanetary features so as to infer terrestrial event properties from their solar sources. A collateral result from studying this database is that CMEs and MCs resulting from erupting sigmoids seem not to adhere to rules such as leading Bz versus solar dipole orientation and, as such, form a distinct class of events. % Instead of a large-scale dipole rule, we find there is a weak (3:2) solar cycle (Hale polarity)-based rule for leading interplanetary field in MCs. We find that the helicity of magnetic clouds is much more strongly correlated (>90%) with launch hemisphere than the 60--70%\ rule of photospheric active region helicity. This rule appears to hold for all CMEs, taking the 28 years of events of Bothmer &\ Rust [``Coronal Mass Ejections,'' AGU Monograph Series 99, 139, 1997]. % At least half of Bothmer &\ Rust's events are associated with disparitions brusques, outside active regions. We therefore suggest that active region sigmoids and disappearing filaments are the origins of two different classes of CMEs.

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