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The X-ray signature of solar coronal massThe coronal response to six solar X-ray flares has been investigated. At a time coincident with the projected onset of the white-light coronal mass ejection associated with each flare, there is a small, discrete soft X-ray enhancement. These enhancements (precursors) precede by typically about 20 m the impulsive phase of the solar flare which is dominant by the time the coronal mass ejection has reached an altitude above 0.5 solar radii. Motions of hot X-ray emitting plasma, during the precursors, which may well be a signature of the mass ejection onsets, are identified. Further investigations have also revealed a second class of X-ray coronal transient, during the main phase of the flare. These appear to be associated with magnetic reconnection above post-flare loop systems.
Document ID
19860025478
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Harrison, R. A. (Birmingham, University United Kingdom)
Waggett, P. W. (Birmingham Univ. United Kingdom)
Bentley, R. D. (London, University College, Dorking, United Kingdom)
Phillips, K. J. H. (SERC Rutherford Appleton Laboratory, Didcot, United Kingdom)
Bruner, M. (Lockheed Research Laboratories Palo Alto, CA, United States)
Date Acquired
August 12, 2013
Publication Date
June 1, 1985
Publication Information
Publication: Solar Physics
Volume: 97
ISSN: 0038-0938
Subject Category
SOLAR PHYSICS
Funding Number(s)
CONTRACT_GRANT: NASA ORDER W-15361
PROJECT: AF PROJECT RESD-84-619
Distribution Limits
Public
Copyright
Other