Volume 416, Number 2, March III 2004
|Page(s)||765 - 773|
|Published online||27 February 2004|
Improved data for solar flare X-ray spectral analysis
National Research Council Senior Research Associate, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
2 Space Science and Technology Dept., Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX, UK
3 Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK
4 Observatoire de Paris–Meudon, Place Jules Janssen, 92195 Meudon, France
5 EURATOM/UKAEA Fusion Association, Culham Science Centre, Abingdon, Oxon OX14 3DB, UK
Corresponding author: K. J. H. Phillips, firstname.lastname@example.org
Accepted: 10 November 2003
The inclusion of collisional rates for He-like Fe and Ca ions is discussed with reference to the analysis of solar flare and line emission, particularly from the Yohkoh Bragg Crystal Spectrometer (BCS). The new data are a slight improvement on calculations presently used in the BCS analysis software in that the discrepancy in the y and z line intensities (observed larger than predicted) is reduced. Values of electron temperature from satellite-to-resonance line ratios are slightly reduced (by up to 1 MK) for a given observed ratio. The new atomic data will be incorporated in the Yohkoh BCS databases. The data should also be of interest for the analysis of high-resolution, non-solar spectra expected from the Constellation-X and Astro-E space missions. A comparison is made of a tokamak spectrum with a synthetic spectrum using atomic data in the existing software and the agreement is found to be good, so validating these data for particularly high-n satellite wavelengths close to the resonance line. An error in a data file used for analyzing BCS spectra is corrected, so permitting analysis of these spectra.
Key words: Sun: flares / Sun: X-rays, gamma rays / X-rays: spectra
© ESO, 2004
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