Coronal Diagnostics Spectrometer Observations of Coronal Loops

Details Coronal Diagnostics Spectrometer Observations of Coronal Loops Coronal Diagnostics Spectrometer Observations of Coronal Loops

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9122n&link_type=abstract

American Astronomical Society Meeting 210, #91.22; Bulletin of the American Astronomical Society, Vol. 39, p.207

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Two side by side loops from the solar disk were analyzed. These two loops were observed with the Coronal Diagnostics Spectrometer on SOHO on 2003 January 17. The first loop was best seen in Mg IX at a wavelength of 368 angstroms and a peak formation temperature of Log T = 6.0. Seven pixels on the loop and one background pixel were chosen. The intensity of the background pixel was subtracted from each of the loop pixels. Only the lines that had a significant intensity after background subtraction were considered. A differential emission measure (DEM) curve was constructed for the background subtracted data using the forward folding technique. The DEM for most of these pixels had a spike shape at Log T equal to 5.85. This result shows that the loop is isothermal at most of these pixels. The second loop was best seen in Si XII at a wavelength of 520 angstroms and a peak formation temperature of Log T = 6.3. The same procedure was followed for the data analysis. After background subtraction only some hot lines had a significant intensity and a DEM curve was constructed for each loop pixel. This time the DEM is broader with a shape that shows that the loop plasma is multithermal with a log temperature range of 6.1 to 6.5.
Solar physics research at the University of Memphis is supported by NSF ATM-0402729 and NASA NNG05GE68G.

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