Non-unique solutions to the stellar atmosphere problem

Details Non-unique solutions to the stellar atmosphere problem Non-unique solutions to the stellar atmosphere problem

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...155..172m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 155, no. 1, Jan. 1986, p. 172-174.

Astronomy and Astrophysics

Astrophysics

24

Carbon Monoxide, Radiative Transfer, Stellar Atmospheres, Stellar Temperature, Surface Temperature, Dynamic Models, Hydrodynamic Equations, Temperature Gradients

Scientific paper

The temperature sensitivity of CO molecular opacity can lead to a bifurcation in the solutions to the stellar atmosphere problem. Models produced with 2-frequency radiative hydrodynamic calculations show that for solar gravity and Teff = 5800 to 5890K, an atmosphere in radiative equilibrium can exist either in a warm phase with a structure like a grey atmosphere or in a distinctly different cool phase. The difference in surface temperature between two such cases at the same Teff amounts to 1000 to 1500K. These temperature differences occur only at elevations some 500 km or more above τRoss = 1.

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