Observations of the 24 September 1997 Coronal Flare Waves

Details Observations of the 24 September 1997 Coronal Flare Waves Observations of the 24 September 1997 Coronal Flare Waves

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000soph..193..161t&link_type=abstract

Solar Physics, v. 193, Issue 1/2, p. 161-180 (2000).

Physics

78

Scientific paper

We report coincident observations of coronal and chromospheric `flare wave' transients in association with a flare, large-scale coronal dimming, metric radio activity and a coronal mass ejection. The two separate eruptions occurring on 24 September 1997 originate in the same active region and display similar morphological features. The first wave transient was observed in EUV and Hα data, corresponding to a wave disturbance in both the chromosphere and the solar corona, ranging from 250 to approaching 1000 km s^-1 at different times and locations along the wavefront. The sharp wavefront had a similar extent and location in both the EUV and Hα data. The data did not show clear evidence of a driver, however. Both events display a coronal EUV dimming which is typically used as an indicator of a coronal mass ejection in the inner corona. White-light coronagraph observations indicate that the first event was accompanied by an observable coronal mass ejection while the second event did not have clear evidence of a CME. Both eruptions were accompanied by metric type II radio bursts propagating at speeds in the range of 500-750 km s^-1, and neither had accompanying interplanetary type II activity. The timing and location of the flare waves appear to indicate an origin with the flaring region, but several signatures associated with coronal mass ejections indicate that the development of the CME may occur in concert with the development of the flare wave.

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