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A Method of Improving Standard Stellar Luminosities with Multiband Standard Bolometric Corrections

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Bakış V. , Eker Z.

tom Vol. 72, No. 3

195--232

Standard luminosity (L) of 406 main-sequence stars with the most accurate astrophysical parameters are calculated from their absolute magnitudes and bolometric corrections at Johnson BV, and Gaia EDR3 G, GBP, GRP filters. Required multiband BC and BC-Teff relations are obtained first from the parameters of 209 Double-lined Detached Eclipsing Binaries with main-sequence components and Gaia EDR3 parallaxes. A simplified SED is formulated to give filter dependent component light contributions and interstellar dimming, which are essential in computing BC of a component, virtually at any filter. The mean standard L of a star is calculated from the mean Mbolwhich is a mathematical average of independent Mboll values predicted at different filters, while the uncertainty of L is the uncertainty propagated from the uncertainty of the mean Mbol. The mean standard L of the sample stars are compared to the corresponding L values according to the Stefan-Boltzmann law. A very high correlation (R2>0.999) is found. Comparing histogram distributions of errors shows that uncertainties associated with the mean standard L (peak at ≈2.5 per cent) are much smaller than the uncertainties of L (peak at ≈8 per cent) by the Stefan-Boltzmann law. Increasing the number of filters used in predicting the mean Mbol increases the accuracy of the standard stellar luminosity. Extinction law, color-color relations and color excess vs. color excess relations for Gaia passbands are presented for the first time for main-sequence stars.