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Causes of extremely fast CMEs

Published online by Cambridge University Press:  01 November 2006

Joan Feynman  and
Alexander Ruzmaikin
Joan Feynman
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA email: Joan.Feynman@jpl.nasa.gov
Alexander Ruzmaikin
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA email: Joan.Feynman@jpl.nasa.gov
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Abstract

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We study CMEs observed by LASCO to have plane of the sky velocities exceeding 1500 km/sec. We find that these extremely fast CMEs are typically associated with flares accompanied by erupting prominences. Our results are consistent with a single CME initiation process that consists of three stages. The initial stage is brought about by the emergence of new magnetic flux, which interacts with the pre-existing magnetic configuration and results in a slow rise of the magnetic structure. The second stage is a fast reconnection phase with flaring, filament eruption and a sudden increase of the rise velocity of the magnetic structure (CME). The third stage consists of propagation in the corona. We discuss the sources of these CMEs and the need for improved understanding of the first and third stages.

Keywords

Sun:coronal mass ejections (CMEs)Sun: prominencesSun: flaresSun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 343 - 346
Copyright
© 2006 International Astronomical Union