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.
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Harrison, R.A., Waggett, P.W., Bentley, R.D. et al. The X-ray signature of solar coronal mass ejections. Sol Phys 97, 387–400 (1985). https://doi.org/10.1007/BF00165998
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DOI: https://doi.org/10.1007/BF00165998