Volume 420, Number 3, June IV 2004
|Page(s)||1047 - 1059|
|Published online||04 June 2004|
Radiative cooling of shocked gas in stellar atmospheres
II. Self-consistent LTE shock wake model with Fe lines and H continua contributions
Institute of Astronomy of the Russian Academy of Sciences, 48 Pjatnitskaya Str., Moscow 109017, Russia
2 Isaak Newton Institute Moscow Branch
3 CRAL, UMR 5574 du CNRS, École Normale Supérieure de Lyon, 46 allée d'Italie, 69364 Lyon Cedex 07, France
4 Observatoire de Haute Provence, CNRS, 04870 Saint Michel l'Observatoire, France
Corresponding author: D. Gillet, firstname.lastname@example.org
Accepted: 13 January 2004
The hot radiative shock wake structure, including the radiative cooling due to H continuum and the Fe lines under typical conditions of stellar atmospheres, is considered. The proposed iterative method of calculation is stable and gives the temperature profile with a good precision (2–5%). The dependence of the wake structure on the preshock parameters is studied, and the line cooling is compared to that of continua in a more self-consistent way. We confirm that the iron cooling is very efficient for low preshock densities (less or equal to 10-11 g/cm3 for Population I, and less or equal to 10-12 g/cm3 for Population II). However, for higher densities, 10-10 g/cm3 and more, especially for the Population II composition, the line cooling becomes secondary with respect to the continuum. As a consequence, the iron cooling is expected to be efficient for pulsating stars having low ratios, like classical Cepheids or RR Lyrae, and much less efficient for W Vir, RV Tauri and Miras. This is discussed in view of the well-known drastic difference in the observed emission features between these two stellar groups.
Key words: shock waves / stars: oscillations / stars: atmospheres
© ESO, 2004
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