Akademik Veri Yönetim Sistemi
ASTRONOMICAL JOURNAL, cilt.171, sa.1, 2026 (SCI-Expanded, Scopus)
A method of obtaining bolometric corrections (BCV) from observed high-resolution, high signal-to-noise spectra is described. The method is applied to the spectra of 128 stars collected from the literature with well-determined effective temperatures (Teff) with the S lambda(V) transparency profiles of Bessell and Landolt. The computed BCV values are found to be accurate within several millimagnitudes, and the effect of different S lambda(V) values is found to be no more than 0.015 mag. The measured visual-to-bolometric ratio (LV/L) from the sample spectra and classically determined BCV from bolometric (MBol) and visual (MV) absolute magnitudes helped us to determine the zero-point constant (C2) of the BCV scale. The determined C2 for each star for each S lambda(V) profile revealed C2 = 2.3653 +/- 0.0067 mag if the S lambda(V) profile of Bessell is used and C2 = 2.3826 +/- 0.0076 mag if the S lambda(V) profile of Landolt is used. Expanding CBol = 71.197425... mag and cBol = - 18.997351... mag announced by IAU2015GARB2, and using the definition of C2 = CBol-CV = cBol-cV, where capital C is the absolute magnitude and lowercase c is the apparent magnitude and subscripts indicate bolometric and visual, the zero-point constants-CV = 68.8321 +/- 0.0067 mag and cV = -21.3627 +/- 0.0067 mag, if LV and are in SI units-were determined corresponding to S lambda(V) of Bessell. The zero-point constants corresponding to S lambda(V) of Landolt are smaller, but the difference is not more than 0.02 mag. Typical and limiting accuracies for predicting a stellar luminosity from an apparent magnitude and a distance are analyzed.