Fe XXI emission line ratios as electron temperature diagnostics for the coronae of cool stars
✍ Scribed by F. P. Keenan; V. J. Foster; K. M. Aggarwal; K. G. Widing
- Publisher
- Springer
- Year
- 1996
- Tongue
- English
- Weight
- 355 KB
- Volume
- 169
- Category
- Article
- ISSN
- 0038-0938
No coin nor oath required. For personal study only.
✦ Synopsis
A comparison of these with observational data lot the 1973 December 17 solar flare, obtained by the Naval Research Laboratory's $082A and S082B spectrographs on board AYolab, reveals reasonably good agreement between theory and observation tot/r [= I(242.07 J')/I(1354.08 ,.' ~.)q_.. which provides some support for the accuracy of the atomic data adopted in the line ratio calculations.
However, our results for R,._ indicate thai the emission feature in Ilare spectra a! 338.06 z~, previously identified as the Fe XXl 2s::2p 2 " Pi -2sZ2P 2 ~,5" line, is not due to this species bul .may be the Ca v 3p a ~P~ -3p33d 31)2 transil:ion. The potential of using /~j as an electron temperature diagnostic for the Fe XXl line emitting regions of cool slat coronae, through a combination of Lvlreme UIt/zn.,iolel Lrplorer and Hubble Space Telescope observations, is briefly disct,ssed.