Spherically symmetric model atmospheres using approximate lambda operators. 1: First results for static non-local thermodynamic equilibrium (NLTE) atmospheres

Details Spherically symmetric model atmospheres using approximate lambda operators. 1: First results for static non-local thermodynamic equilibrium (NLTE) atmospheres Spherically symmetric model atmospheres using approximate lambda operators. 1: First results for static non-local thermodynamic equilibrium (NLTE) atmospheres

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...287..179k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 287, no. 1, p. 179-190

Mathematics

18

B Stars, O Stars, Operators (Mathematics), Radiative Transfer, Stellar Atmospheres, Stellar Models, Symmetry, Approximation, Electron Scattering, Iterative Solution, Linearization, Measure And Integration, Optical Thickness, Ray Tracing, Statistical Analysis, Thermodynamic Equilibrium

Scientific paper

A method for calculation of static spherically symmetric non-local thermodynamic equilibrium (NLTE) model atmospheres is presented. The accelerated lambda iteration (ALI) technique is used. The radiative transfer equation is incorporated into the constraint equations of hydrostatic, radiative, and statistical equilibrium. The equations of statistical equilibrium are linearized implicitly. In addition, the Rosseland optical depth equation is also solved, allowing for changes of the radial distance from iteration to iteration. The resulting system may be solved using two methods, namely via a linearization, or with the help of a depth integration. Detailed expressions for linearization coefficients are presented in Appendix. The formal solution of the radiative transfer equation is calculated using a ray method. Test calculations of the model atmosphere for an O star with L = 1.25 x 106 solar luminosity, R = 24 solar radius and M = 60 solar mass are presented. Results of our calculations are compared with previously published models that were calculated using a complete linearization method. The convergence of the method is tested for two model calculations. Our method yields faster convergence for a B star than for an O star, since the opacity in an O star atmosphere is dominated by electron scattering.

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