Predicted magnitudes and colors from cool-star model atmospheres

Details Predicted magnitudes and colors from cool-star model atmospheres Predicted magnitudes and colors from cool-star model atmospheres

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982saosr.392a.239j&link_type=abstract

In Smithsonian Astrophysics Observatory 2nd Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, Vol. 1 p 239-244 (

Astronomy and Astrophysics

Astrophysics

1

Color, Predictions, Stellar Atmospheres, Stellar Magnitude, Supergiant Stars, Black Body Radiation, Calibrating, Comparison, K Stars, Stellar Models, Temperature Dependence

Scientific paper

An intercomparison of model stellar atmospheres and observations of real stars can lead to a better understanding of the relationship between the physical properties of stars and their observed radiative flux. In this spirit we have determined wide-band and narrow-band magnitudes and colors for a subset of models of K and M giant and supergiant stars selected from the grid of 40 models by Johnson, Bernat and Krupp (1980) (hereafter referred to as JBK). The 24 models selected have effective temperatures of 4000, 3800, 3600, 3400, 3200, 3000, 2750 and 2500 K and log g = 0, 1 or 2. Emergent energy fluxes (erg/ sq cm s A) were calculated at 9140 wavelengths for each model. These computed flux curves were folded through the transmission functions of Wing's 8-color system (Wing, 1971; White and Wing, 1978) and through Johnson's (1965) wide-band (BVRIJKLM) system. The calibration of the resultant magnitudes was made by using the absolute calibration of the flux curve of Vega by Schild, et al. (1971).

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