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Plasma dynamics of a prominence associated coronal mass ejection

Published online by Cambridge University Press:  14 March 2005

D. Tripathi ,
V. Bothmer ,
S. K. Solanki ,
R. Schwenn ,
M. Mierla  and
G. Stenborg
D. Tripathi
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany email: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]
V. Bothmer
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany email: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]
S. K. Solanki
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany email: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]
R. Schwenn
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany email: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]
M. Mierla
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany email: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]
G. Stenborg
Affiliation:
NASA Goddard Space Flight Center, Greenbelt, USA Catholic University of America, USA email: [email protected]
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Abstract

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An erupting prominence seen by SOHO/EIT was tracked into the field of view of the LASCO C2 and C3 coronagraphs where it developed into the core of a structured CME. The erupting prominence was deflected by an angle of $\sim 20^{\circ}$ towards the north pole whereas the consequent core of the CME and it's leading edge propagated in the outer corona at constant position angle. The prominence material underwent a constant acceleration phase until a height of $\sim$1.5 solar radii before it started to decelerate up to a distance of 5.0 solar radii. An inflow of plasma with a speed of about 70-80 km/s was discovered in the EIT observations at a height of 1.5-1.2 solar radii in the course of the prominence eruption, matching in time the prominence deceleration phase. The downflowing material followed a curved path, suggestive of the apex of a contracting magnetic loop sliding down along other field lines.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS223 , June 2004 , pp. 401 - 402
Copyright
© 2004 International Astronomical Union