Deriving the Density and Ionization Profile along Flaring Loop

Details Deriving the Density and Ionization Profile along Flaring Loop Deriving the Density and Ionization Profile along Flaring Loop

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.2230s&link_type=abstract

American Astronomical Society, SPD meeting #42, #22.30; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Determining the evolution of the chromospheric and coronal plasma during a solar flare is a key step in understanding how this plasma responds to heating from nonthermal electrons or other sources, and in identifying the source(s) and location of heating.
We develop a method to derive the density structure of local plasma along flaring loops using nonthermal X-ray observations. The method is based on the relationship between emission and column density derived from our simple nonuniform ionization thick-target model (Su et al. 2011). A similar idea was presented by Leach and Petrosian (1981) and was applied to Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) observations of one flare by Liu et al. (2006). This method does not require an assumed density structure, unlike other methods (Aschwanden et al. 2002, Prato et al. 2009, Kontar et al. 2008 and Saint-Hilaire et al. 2010) which use the peak or centroid positions of X-ray sources in different energy bands and an assumed form for the density structure.
Our method also determines the location of the transition layer between ionized and neutral gas, a new result in flare studies. Our preliminary results show an increase in the density of the loop top and an decrease in the height of the transition layer. These agree with the standard flare model and chromospheric evaporation. Using this method to derive the time evolution of density and ionization structure, we will compare our results with chromospheric evaporation models (Allred et al. 2005).

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