Imaging Spectroscopy Of Chromospheric Evaporation During An X-class Flare Using Rhessi And Soho/cds

Details Imaging Spectroscopy Of Chromospheric Evaporation During An X-class Flare Using Rhessi And Soho/cds Imaging Spectroscopy Of Chromospheric Evaporation During An X-class Flare Using Rhessi And Soho/cds

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9302m&link_type=abstract

American Astronomical Society Meeting 210, #93.02; Bulletin of the American Astronomical Society, Vol. 39, p.211

Astronomy and Astrophysics

Astronomy

Scientific paper

Here we present observations of chromospheric evaporation lasting 1 hour during an X1.5 flare using RHESSI and SOHO/CDS datasets. Our study focuses on comparing upflow velocities measured with an 10 minute cadence in the 8 MK Fe XIX line using CDS, with co-spatial and co-temporal HXR emission observed with RHESSI. The magnitude of this event enables the footpoints to be spatially resolved by both instruments. This allows the use of imaging spectroscopy to monitor both the electron beam parameters and the evolution of the heated chromospheric material for each footpoint at given intervals (every 10 minutes due to the rastering nature of CDS) throughout the event. Our preliminary findings show that the HXR emission observed by RHESSI is divided into two distinct phases: an initial 'bursty' phase, which we interpret as accelerated electrons being beamed directly down to the footpoints, followed by a period of more gradually varying emission, which we interpret as high-energy electrons leaking out of a magnetic trap. It is only during the initial phase that significant evaporation is observed by CDS, despite the presence of up to 250 keV emission during the gradual phase.

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