EDP Sciences
Free access
Volume 487, Number 3, September I 2008
Page(s) 1203 - 1208
Section Atomic, molecular, and nuclear data
DOI http://dx.doi.org/10.1051/0004-6361:200809998
Published online 24 June 2008

A&A 487, 1203-1208 (2008)
DOI: 10.1051/0004-6361:200809998

Electron-impact excitation of Be-like Mg

G. Del Zanna1, 2, I. Rozum1, and N. R. Badnell3

1  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

Received 17 April 2008 / 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 n=4. We find significant differences with the widely used n=2 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