Incorporating the atmosphere in stellar structure models: the solar case

Details Incorporating the atmosphere in stellar structure models: the solar case Incorporating the atmosphere in stellar structure models: the solar case

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286...91m&link_type=abstract

Astronomy and Astrophysics 286, 91-102 (1994)

Astronomy and Astrophysics

Astrophysics

44

Stars: Evolution, Stars: Atmosphere, Stars: Interiors, Sun: Interior, Sun: Oscillations

Scientific paper

The diffusion limit of the transfer equation used in the calculations of stellar interior models is only valid at large Rosseland optical depth. From atmosphere models obtained with ATLAS 9 (Kurucz), it is shown here that the diffusion limit of the transfer equation becomes valid only at Rosseland optical depths τ_R_ >~ 10 that is at a location well inside the Sun's convective zone. For the calculations of stellar evolution, the atmosphere is built from T(τ) laws that are derived either from theory or from full atmosphere computations; such a T(τ) law depends upon effective temperature and gravity, therefore on the evolutionary state of the model. Hence, in general, when following the evolution of a star, various T(τ) laws need to be introduced. In the case of the Sun, however, we show here that the atmosphere can be restored with the use of only one T(τ) law. Particular efforts have been made to include physics as consistent as possible in both the model atmosphere from which one derives T(τ) laws and the internal structure calculations which use them; as a result, we can rebuild the atmosphere in stellar models with an accuracy of about +/- 0.5% for the sound speed and the pressure. Remaining discrepancies are of small effect on solar calibrated models. For the solar oscillations, such small discrepancies generate frequency differences no larger than 2μHz for low degrees modes to about 10μHz for modes of large degrees around 400.

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