\journalname
Astronomy&AstrophysicsReview
Testing and applying the calibrations.
In principle, the above calibrations allow one to infer the mass and radius of a single star to a few per cent from an observed set of accurate values of \(T_{\rm eff}\), \(\log g\) and [Fe/H]. For example, when applied to the Sun itself, the results are \(M=1.051~{}M_{\odot}\) and \(R=1.018~{}R_{\odot}\), well within the scatter of the calibrations. These relations are particularly interesting for exoplanet host stars, where the properties of the planet are normally obtained relative to those of the star. We have therefore checked the results of our purely empirical calibrations with the set of results obtained for the host stars of transiting planets by \cite{GT08}. For such stars, additional information about the radius and \(\log g\) is available from the transit light curves, and masses are then inferred from stellar evolution models. The results of the comparison are shown in Fig. \ref{CalibTest1}, and the agreement is very satisfactory.