| Issue |
A&A
Volume 432, Number 3, March IV 2005
|
|
|---|---|---|
| Page(s) | 1137 - 1150 | |
| Section | Atomic, molecular, and nuclear data | |
| DOI | https://doi.org/10.1051/0004-6361:20041849 | |
| Published online | 07 March 2005 | |
Benchmarking atomic data for astrophysics:
*
Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge CB3 0WA, UK e-mail: G.Del-Zanna@damtp.cam.ac.uk
Received:
16
August
2004
Accepted:
29
November
2004
Recent scattering calculations for are
benchmarked against laboratory and astrophysical observations.
The collisional data are supplemented by radiative data
obtained with empirical adjustments that
take into account observed wavelengths.
All previous line identifications and energy levels
are reviewed and assessed in light of these new calculations.
Most of the previous identifications, in particular of the
astrophysically-important spectral lines are confirmed.
However, some identification are rejected or questioned, and new ones
proposed.
The agreement between theoretical and experimental data
in terms of wavelengths, line intensities and level lifetimes
is very good.
Observations of L-shell emission lines provide a
great opportunity to directly measure electron temperatures
for a wide range of astrophysical sources.
Examples from solar (SMM, SOLEX) and stellar (Chandra, EUVE)
observations are provided.
Key words: atomic data / line: identification / Sun: corona / techniques: spectroscopic
© ESO, 2005
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