Radiative cooling of shocked gas in stellar atmospheres. II. Self-consistent LTE shock wake model with Fe lines and H continua contributions

Details Radiative cooling of shocked gas in stellar atmospheres. II. Self-consistent LTE shock wake model with Fe lines and H continua contributions Radiative cooling of shocked gas in stellar atmospheres. II. Self-consistent LTE shock wake model with Fe lines and H continua contributions

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...420.1047f&link_type=abstract

Astronomy and Astrophysics, v.420, p.1047-1059 (2004)

Astronomy and Astrophysics

Astrophysics

3

Shock Waves, Stars: Oscillations, Stars: Atmospheres

Scientific paper

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 R/M 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.

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