Fe XXV temperatures in flares from the YOHKOH Bragg crystal spectrometer

Details Fe XXV temperatures in flares from the YOHKOH Bragg crystal spectrometer Fe XXV temperatures in flares from the YOHKOH Bragg crystal spectrometer

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...435..898s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 435, no. 2, p. 898-908

Astronomy and Astrophysics

Astrophysics

10

Flux Density, Iron, Line Spectra, Resonant Frequencies, Solar Flares, Solar Temperature, Scientific Satellites, Solar Spectrometers, Statistical Distributions

Scientific paper

Studies by Doschek et al. using P78-1 and Solar Maximum Misson (SMM) data have shown that the ratio of intensities of the Fe XXV and Ca XIX resonance lines can be expressed as a function of Fe XXV temperature. Using a more recent data set consisting of 13 flares observed by the Bragg crystal spectrometer (BCS) experiment on board Yohkoh, we find a nearly identical functional relationship between the same resonance line ratios and Fe XXV temperatures. We use this functional relationship to obtain resonance line ratio temperatures (TRLR) for each flare in our data set, and compare them with temperatures resulting from application of a simple spectral fitting method. (TSSF) to individal Fe XXV spectra. We also use a more involved free-parameter spectral fitting method to deduce temperatures (TFSF) from some of these spectra. On average, agreement between TRLR and TSSF improves as a flare progresses in time, with average agreements of 10.0% +/- 5.2%, 6.4% +/- 5.4%, and 5.0% +/- 3.9% over the rise, peak, and decay phases, respectively. Deviations between TRLR and TFSF are about the same or smaller. Thus, for most analysis purposes, all three methods yield virtually identical temperatures in flares. The somewhat poorer agreement between TSSF and TRLR during the earlier phases may be partially a result of difficulties in obtaining precise values for temperatures from spectral fits when blueshifts and large nonthermal broadenings are present in the spectra. Because of the high sensitivity of the Yohkoh BCS compared to that of BCS experiments on earlier spacecraft, we can for the first time consistently observe the heating phase of flares in Fe XXV.

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