The CO/SiO radiative instability in cool star atmospheres revisited

Details The CO/SiO radiative instability in cool star atmospheres revisited The CO/SiO radiative instability in cool star atmospheres revisited

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...433..303c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 433, no. 1, p. 303-312

Astronomy and Astrophysics

Astrophysics

21

Cool Stars, Late Stars, Radiative Transfer, Stellar Atmospheres, Stellar Envelopes, Stellar Models, Stellar Temperature, Thermal Stability, Atmospheric Models, Carbon Monoxide, Hydrodynamics, Mathematical Models, Molecular Dynamics, Silicon Oxides

Scientific paper

We revisit the formation of radiative instabilities in cool star atmospheres and compare our results with those given by Muchmore, Nuth, & Stencel. We have considered the combined influence of CO and SiO molecules and have computed models for a grid of effective temperatures and geometrical dilution factors for the stellar radiation. Our results are based on the analysis of the energy balance of gas elements with prescribed thermodynamic properties. Our results show that radiative instabilities are most likely primarily caused by CO, whereas SiO is expected to play only a minor role, except when the CO density is reduced compared to Local Thermodynamic Equilibrium (LTE) values or the CO band can be assumed to be optically thick. The onset of radiative instabilities is expected to be strongly modified when dynamic phenomena such as stochastic shocks are present. Our results provide strong evidence that dust formation can most likely occur via a radiative instability alone. Therefore, we present a revised version of the Muchmore et al. dust formation paradigm, which also considers hydrodynamic cooling. The new paradigm is particularly relevant in cases where dust is formed relatively close to the stellar photosphere.

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