Flare Temperature from FE XXV and CA XIX: Improved Atomic Data

Details Flare Temperature from FE XXV and CA XIX: Improved Atomic Data Flare Temperature from FE XXV and CA XIX: Improved Atomic Data

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..293p&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Computer Science

Scientific paper

For several years flare temperatures and emission measures have been derived from comparison of observed Yohkoh BCS spectra with theoretical spectra derived from atomic parameters based on distorted wave approximation. In the case of Fe XXV and Ca XIX spectra, the main lines used in the determination are dielectronic satellite lines (j or k as appropriate) and the resonance line w. More accurate close-coupling calculations from the R-matrix procedure have been available in unpublished form, and in this work these new atomic data were substituted for the distorted wave data. The intensities of the Fe XXV and Ca XIX lines w, x, y, and z are affected -- all are increased. However, the differences from the previously used atomic data are very slight. We estimate that for a given j/w ratio in Fe XXV, for instance, the temperature estimated from the new atomic data will be about 1MK smaller than from the existing data in the standard Yohkoh software at temperatures of around 20MK. Smaller differences are expected for Ca XIX at typical temperatures of 14MK. The increase in the Fe XXV y and z line intensities tends to reduce a well-known discrepancy in these lines (more evident in the much better resolved SMM BCS spectra) but not by a sufficient amount to explain the discrepancy.

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