On the Dynamic Stability of Cool Supergiant Atmospheres

Details On the Dynamic Stability of Cool Supergiant Atmospheres On the Dynamic Stability of Cool Supergiant Atmospheres

2001-06-28

arxiv.org/abs/astro-ph/0106547v1

Astronomy and Astrophysics

Astrophysics

54 pages including figures and the Appendix, 7 figures, Accepted for The Astrophysical Journal, Main Journal, 558, Sept. 2001

Scientific paper

10.1086/322476

We have developed a new formalism to compute the thermodynamic coefficient Gamma1 in the theory of stellar and atmospheric stability. We generalize the classical derivation of the first adiabatic index, which is based on the assumption of thermal ionization and equilibrium between gas and radiation temperature, towards an expression which incorporates photo-ionization due to radiation with a temperature T_rad different from the local kinetic gas temperature.Our formalism considers the important non-LTE conditions in the extended atmospheres of supergiant stars. An application to the Kurucz grid of cool supergiant atmospheres demonstrates that models with T_rad =~ T_eff between 6500 K and 7500 K become most unstable against dynamic perturbations, according to Ledoux' stability integral . This results from Gamma1 and acquiring very low values, below 4/3, throughout the entire stellar atmosphere, which causes very high gas compression ratios around these effective temperatures. Based on detailed NLTE-calculations, we discuss atmospheric instability of pulsating massive yellow supergiants, like the hypergiant rho Cas (Ia+), which exist in the extension of the Cepheid instability strip, near the Eddington luminosity limit.

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