Abstract
The scales of the effective temperature T eff and bolometric correction (BC) are necessary for isochrones to be compared with observed colour—magnitude diagrams (CMDs) of star clusters. Reliable scales can be found, providing improved numerical relations between observed and theoretical quantities. A detailed analysis is presented of the effects which the log T eff, B−V and BC scales have on the transformation of evolutionary tracks and time isochrones from the theoretical Hertzsprung—Russell diagram to the CMD. We present a comparison between different scales of published transformations to find the ages of some selected open clusters.
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