Volume 487, Number 3, September I 2008
|Page(s)||1203 - 1208|
|Section||Atomic, molecular, and nuclear data|
|Published online||24 June 2008|
Electron-impact excitation of Be-like Mg*
MSSL, University College London, Holmbury St., Mary, Dorking RH5 6NT, UK e-mail: G.Del-Zanna@damtp.cam.ac.uk;GDelZanna@spd.aas.org
2 DAMTP, Centre for Mathematical Sciences, Wilberforce road, Cambridge CB3 0WA, UK
3 Department of Physics, University of Strathclyde, Glasgow G4 0NG, UK
Accepted: 13 June 2008
We present an R-matrix calculation of electron-impact excitation of Be-like Mg. The calculation is similar to that one presented for Be-like Fe by Chidichimo et al. (2005, A&A, 430, 331), and was done with the intermediate-coupling frame transformation method and including a total of 98 fine-structure levels, up to . We find significant differences with the widely used excitation rates of Keenan et al. (1986, Phys. Scr., 34, 216), calculated by interpolating R-matrix calculations along the Be-like sequence. We present a list of the most important transitions and a few comparisons with SOHO SUMER and CDS/GIS spectra of the solar corona. We show that previous long-standing discrepancies between observed and predicted line intensities are now resolved. We also show how temperatures of the solar corona were significantly underestimated. For example, a coronal hole inter-plume temperature of 850 000 K found by Wilhelm et al. (1998, ApJ, 500, 1023) is now revised to 1 160 000 K.
Key words: atomic data / techniques: spectroscopic / Sun: corona
© ESO, 2008
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