Model atmospheres for G, F, A, B, and O stars

Abstract

A grid of LTE model atmospheres is presented for effective temperatures ranging from 5500 to 50,000 K, gravities from the main sequence down to the radiation-pressure limit, and abundances solar, 1/10 solar, and 1/100 solar. The models were computed by use of a statistical distribution-function representation of the opacity of almost a million atomic lines. For each model the temperature structure, fluxes, UBV and uvby colors, bolometric correction, and Balmer line profiles are tabulated. The solar-abundance models are compared with narrow-, intermediate-, and wide-band photometry and found to be in good agreement with the observations for effective temperatures above 8000 K. Excellent agreement exists with the spectrophotometry and Balmer line profiles of Vega. A small systematic error in the colors of late A and F stars is probably due to an overstimate of convection in weakly convective models. This error does not seem to affect greatly the use of the predicted colors for differential studies. The solar model has approximately a 2% error in the V flux because molecular lines were not included.