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CME Interaction and the Intensity of Solar Energetic Particle Events

Published online by Cambridge University Press:  03 June 2005

N. Gopalswamy ,
S. Yashiro ,
S. Krucker  and
R. A. Howard
N. Gopalswamy
Affiliation:
Code 695.0, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA email: [email protected]
S. Yashiro
Affiliation:
Code 695.0, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA email: [email protected] Department of Physics, The Catholic University of America, Washington, DC 20064, USA
S. Krucker
Affiliation:
Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA 94720, USA
R. A. Howard
Affiliation:
Solar Physics Branch, Naval Research Laboratory, Washington, DC, 20375, USA
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Abstract

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Large Solar Energetic Particles (SEPs) are closely associated with coronal mass ejections (CMEs). The significant correlation observed between SEP intensity and CME speed has been considered as the evidence for such a close connection. The recent finding that SEP events with preceding wide CMEs are likely to have higher intensities compared to those without was attributed to the interaction of the CME-driven shocks with the preceding CMEs or with their aftermath. It is also possible that the intensity of SEPs may also be affected by the properties of the solar source region. In this study, we found that the active region area has no relation with the SEP intensity and CME speed, thus supporting the importance of CME interaction. However, there is a significant correlation between flare size and the active region area, which probably reflects the spatial scale of the flare phenomenon as compared to that of the CME-driven shock.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

shock wavesSun: coronal mass ejections (CMEs)Sun: flaresSun: X-raysgamma raysSun: particle emissionsolar-terrestrial relations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS226 , September 2004 , pp. 367 - 373
Copyright
© 2005 International Astronomical Union