Abstract
A method for determining the effective temperature T eff 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 [c 1] index in the uvby system. Empirical relations between the T eff 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 [c 1] indices for these stars, on the other hand, are plotted. A systematic discrepancy between the dependences of T eff 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 T eff value in the range of 3800 ≤ T ≤ 5100 K (based on the Q index) or 4900 ≤ T eff ≤ 5500 K (based on the [c 1] index).
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Original Russian Text © L.S. Lyubimkov, D.B. Poklad, 2014, published in Kinematika i Fizika Nebesnykh Tel, 2014, Vol. 30, No. 5, pp. 56–71.
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Lyubimkov, L.S., Poklad, D.B. Determining the effective temperatures of G- and K-type giants and supergiants based on observed photometric indices. Kinemat. Phys. Celest. Bodies 30, 244–254 (2014). https://doi.org/10.3103/S0884591314050055
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DOI: https://doi.org/10.3103/S0884591314050055