Abstract
A method for determining the effective temperature Teff of G- and K-type giants and supergiants is proposed. The method is based on the use of two photometric indices free from the interstellar absorption influence: the Q index in the UBV photometric system and the [c1] index in the uvby system. Empirical relations between the Teff values found for nearby and bright G- and K-type giants and supergiants with the use of the infrared fluxes method (IRFM), on the one hand, and the observed Q and [c1] indices for these stars, on the other hand, are plotted. A systematic discrepancy between the dependences of Teff on Q for the stars with standard and reduced metallicities is found. Approximating the plotted dependences with second-order polynomials, one can obtain a relatively simple and a rather accurate method for determining the Teff value in the range of 3800 < Teff < 5100 K (based on the Q index) or 4900 < Teff < 5500 K (based on the [c1] index).
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