Evolution of White-Light Flares Observed by YOHKOH

Details Evolution of White-Light Flares Observed by YOHKOH Evolution of White-Light Flares Observed by YOHKOH

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000soph..194..305s&link_type=abstract

Solar Physics, v. 194, Issue 2, p. 305-325 (2000).

Physics

9

Scientific paper

We consider in detail the evolutionary patterns of few white-light flares observed by Yohkoh. The following data have been used in the analysis: sequences of de-convolved SXT images in X-ray and optical filters, MEM reconstructed HXT images and the other supporting data. The resolution in the de-convolved images is below 1 arc sec. Working with sequences of de-convolved images makes it also possible to investigate the dynamics of these structures with high spatial accuracy. Comparison of the morphology of flare brightenings as observed in hard, soft and optical ranges reveals that these emissions are not co-spatial and are most probably related to different plasma volumes at any instant. These observations cannot be easily accommodated within standard flare scenarios. Traditionally, the hard and optical flare emissions are expected to be co-spatial and the soft X-ray emission is presumed to fill the coronal portion of flaring loop(s) during rise phase. Present observations do not easily fit to such scenario.

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