Observational Evidence of Chromospheric Evaporation

Details Observational Evidence of Chromospheric Evaporation Observational Evidence of Chromospheric Evaporation

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0828m&link_type=abstract

American Astronomical Society, SPD meeting #37, #8.28

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Scientific paper

Observational evidence for chromospheric evaporation during the impulsive phase of two solar flares is presented using data from the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) and the Coronal Diagnostic Spectrometer (CDS) on board SOHO. For the first time, co-spatial imaging and spectroscopy have been used to observe both gentle and explosive evaporation processes within HXR emitting regions. For a GOES C9.1 flare, a low flux of non-thermal electrons was found to produce low-velocity upflows in the cool He I and O V emission lines and moderate upflows in the 8 MK Fe XIX line indicative of gentle evaporation. An M2.2 flare, on the other hand, showed low-velocity downflows in the He I and O V lines and high-velocity upflows in the Fe XIX line, for an electron flux value which was an order of magnitude higher, indicative of an explosive process. These findings confirm that the dynamic response of the solar atmosphere is sensitively dependent on the flux of incident electrons as predicted by current hydrodynamical simulations.

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