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Model atmospheres for G, F, A, B, and O stars
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1979
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A grid of LTE model atmospheres covering effective temperatures 5 500–50 000 K, a wide range of gravities, and solar to 1/100 solar abundances is presented. The models were computed with a statistical distribution‑function representation of the opacity of nearly a million atomic lines, yielding tabulated temperature structures, fluxes, UBV/uvby colors, bolometric corrections, and Balmer line profiles. Solar‑abundance models agree well with photometry and spectrophotometry for T_eff > 8000 K, including Vega, but late A and F stars show a small color error from overestimated convection that minimally affects differential studies, and the solar model has a ~2 % V‑flux error due to missing molecular lines. Published in ApJS (May 1979), DOI 10.1086/190589, with extensive tables of atmospheric data for G, F, A, B, and O stars.
view Abstract Citations (3777) References (38) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Model atmospheres for G, F, A, B, and O stars. Kurucz, R. L. 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. Publication: The Astrophysical Journal Supplement Series Pub Date: May 1979 DOI: 10.1086/190589 Bibcode: 1979ApJS...40....1K Keywords: Atmospheric Models; Early Stars; F Stars; G Stars; Line Spectra; Stellar Atmospheres; Stellar Models; A Stars; Abundance; B Stars; Balmer Series; Distribution Functions; Error Analysis; O Stars; Opacity; Radiation Pressure; Solar Atmosphere; Solar Simulation; Spectrophotometry; Statistical Analysis; Tables (Data); Temperature Effects; Astrophysics; A Stars:Atmospheres; Atmospheres:B Stars; Atmospheres:F Stars; Atmospheres:G Stars; Atmospheres:O Stars; Early-Type Stars:Spectrophotometry; Stellar Atmospheres:Models full text sources ADS | data products CDS (2) SIMBAD (1) Related Materials (1) Catalog: 1993yCat.6039....0K