Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12.1123m&link_type=abstract
The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August
Astronomy and Astrophysics
Astrophysics
2
Scientific paper
Helium-like density and temperature diagnostics, since more than three decades applied to the Sun, have now become a powerful tool in the analysis of the high-resolution Chandra and XMM-Newton X-ray spectra. Therefore, we have revisited the calculation of the ratios R=f/i and G=(f+i)/r of the resonance r (1s2 1S0 - 1s2p 1P1), intercombination i (1s2 1S0 - 1s2p 3P2,1), and forbidden f (1s2 1{S}0 - 1s2s 3{S}1) ``triplet'' lines of the He-like ions ion{C}{5}, ion{N}{6}, ion{O}{7}, ion{Ne}{9}, ion{Mg}{11}, and ion{Si}{13}, taking into account all relevant processes and improved atomic data. The first calculations have been done for optically thin plasmas in collisional ionization equilibrium (e.g., stellar coronae). The influence of an external radiation field on the depopulation of the upper level of f is considered which can be important for hot OB or F stars (e.g., ζ Puppis, Procyon, and Algol). In preparation are updated calculations for photo-ionized and hybrid plasmas (e.g., warm absorber in AGNs), and for transient ionization plasmas (young SNRs).
Dubau Jacques
Kaastra Jelle S.
Mewe Rolf
Ness Jan-Use
Porquet Delphine
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