Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...444..305l&link_type=abstract
Astronomy and Astrophysics, Volume 444, Issue 1, December II 2005, pp.305-317
Astronomy and Astrophysics
Astrophysics
2
Atomic Data, Sun: Corona, Sun: Uv Radiation
Scientific paper
Electron impact collision strengths, energy levels, oscillator strengths and spontaneous radiative decay rates are calculated for Ca xiii. The configurations used are {2s2} {2p4}, {2s2p5}, {2p6}, {2s2} {2s3 3s}, {2s2} {2p3 3p} and {2s2}{2p3 3d} giving rise to 86 fine-structure levels in intermediate coupling. Collision strengths are calculated at five incident energies (40, 80, 120, 160 and 200 Ry) in the distorted wave approximation. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates, statistical equilibrium equations for level populations are solved at electron densities covering the range of 108-1014 cm-3 at an electron temperature of log Te(K)=6.5, corresponding to maximum abundance of Ca xiii. Relative and absolute spectral line intensities are calculated, and their diagnostic relevance is discussed. This dataset will be made available in the next version of the CHIANTI database.
Bhatia Anand K.
Landi Enrico
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