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RHESSI and SDO/AIA observations of the chromospheric and coronal plasma parameters during a solar flare View all abstracts by submitter

Marina Battaglia   Submitted: 2012-10-15 01:51

X-ray and EUV observations are an important diagnostic of various plasma parameters of the solar atmosphere during solar flares. Soft X-ray and EUV observations often show coronal sources near the top of flaring loops, while hard X-ray emission is mostly observed from chromospheric footpoints. Combining RHESSI with simultaneous SDO/AIA observations, it is possible for the first time to determine the density, temperature, and emission profile of the solar atmosphere over a wide range of heights during a flare, using two independent methods. Here we analyze a near limb event during the first of three hard X-ray peaks. The emission measure, temperature, and density of the coronal source is found using soft X-ray RHESSI images while the chromospheric density is determined using RHESSI visibility analysis of the hard X-ray footpoints. A regularized inversion technique is applied to AIA images of the flare to find the differential emission measure (DEM). Using DEM maps we determine the emission and temperature structure of the loop, as well as the density, and compare it with RHESSI results. The soft X-ray and hard X-ray sources are spatially coincident with the top and bottom of the EUV loop, but the bulk of the EUV emission originates from a region without co-spatial RHESSI emission. The temperature analysis along the loop indicates that the hottest plasma is found near the coronal loop top source. The EUV observations suggest that the density in the loop legs increases with increasing height while the temperature remains constant within uncertainties.

Authors: Marina Battaglia, Eduard P. Kontar
Projects: RHESSI,SDO-AIA

Publication Status: ApJ, accepted
Last Modified: 2012-10-15 12:44
Go to main E-Print page  Least-Squares Fitting Methods for Estimating the Winding Rate in Twisted Magnetic-Flux Tubes  X-ray and UV investigation into the magnetic connectivity of a solar flare  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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