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Helicity of Magnetic Clouds and Solar Cycle Variations of their Geoeffectiveness

Published online by Cambridge University Press:  03 June 2005

Katya Georgieva  and
Boian Kirov
Katya Georgieva
Affiliation:
Solar-Terrestrial Influences Laboratory at the Bulgarian Academy of Sciences, Bl.3 Acad.G.Bonchev Str, 1113 Sofia, Bulgaria, email: kgeorg@bas.bg
Boian Kirov
Affiliation:
Solar-Terrestrial Influences Laboratory at the Bulgarian Academy of Sciences, Bl.3 Acad.G.Bonchev Str, 1113 Sofia, Bulgaria, email: bkirov@space.bas.bg
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Abstract

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Coronal mass ejections (CMEs) are sources of the strongest geomagnetic disturbances. From sunspot minimum to sunspot maximum, the intensity of storms associated with CMEs increases but the degree of association decreases. We divide the CMEs in the last solar cycle (1996–2002) into magnetic clouds (MCs)and CMEs which are not magnetic clouds. MCs are much more geoeffective than non-MC CMEs, and the portion of CMEs which are MCs is maximum in sunspot minimum and minimum at sunspot maximum, corresponding to the net helicity transferred from the solar interior into the corona. The smaller portion of the more geoeffective MCs is the explanation of the smaller degree of association of CMEs with geomagnetic disturbances in sunspot maximum.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Sun: coronal mass ejections (CMEs)magnetic fieldssolar-terrestrial relations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS226 , September 2004 , pp. 470 - 472
Copyright
© 2005 International Astronomical Union