The X-ray signature of solar coronal mass ejections |
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| Authors: | R A Harrison P W Waggett R D Bentley K J H Phillips M Bruner M Dryer G M Simnett |
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| Institution: | (1) Department of Space Research, University of Birmingham, U.K.;(2) Present address: High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colo., U.S.A.;(3) Mullard Space Science Lab., University College London, U.K.;(4) Rutherford Appleton Lab., Chilton, U.K.;(5) Lockheed Palo Alto Research Labs., Calif., U.S.A.;(6) Space Environment Lab., NOAA-ERL, Boulder, Colo., U.S.A.;(7) Department of Space Research, University of Birmingham, U.K. |
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| Abstract: | The 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  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 R
 . We identify motions of hot X-ray emitting plasma, during the precursors, which may well be a signature of the mass ejection onsets. 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.NCAR is sponsored by the National Science Foundation. |
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