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The Plasma Environment of Prominences – SOHO Observations

Published online by Cambridge University Press:  12 April 2016

D. Moses ,
C.M. Korendyke ,
N. Moulton  and
J. Newmark
D. Moses
Affiliation:
Naval Research Laboratory, Code 7660.1, Washington, DC 20375, USA
C.M. Korendyke
Affiliation:
Naval Research Laboratory, Code 7660.1, Washington, DC 20375, USA
N. Moulton
Affiliation:
Naval Research Laboratory, Code 7660.1, Washington, DC 20375, USA
J. Newmark
Affiliation:
NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA

Abstract

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We describe the observational capabilities of the SOHO EIT and LASCO instruments for prominence research. A detailed comparison of EIT He II λ304 and BBSO Hα images of a quiescent prominence reveals differences in fine scale structure which are attributed to differences in radiation emission and transport mechanisms. Absorption features present in coronal EIT images are attributed to dense prominence features located between the source of the coronal emission and the observer. These features provide the locations of prominence material in coronal image sequences. Observations of a prominence eruption in both EIT He II and LASCO C1 Fe XIV images show the heating of chromospheric material to coronal temperatures during the prominence eruption. In the last phase of the prominence eruption, a coronal mass ejection (CME) is initiated as a dark cavity forms over the prominence material and a bright loop-like structure forms over the dark cavity.

Type
Filaments and Their Environment
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 45 - 54
Copyright
Copyright © Astronomical Society of the Pacific 1998

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