\journalname
Astronomy&AstrophysicsReview
The temperature-mass-radius diagrams.
Fig. \ref{logMlogT} shows the observed \(M\) vs. \(T_{\rm eff}\) for the stars in Table \ref{tableMR}, corresponding roughly to the dependence of mass on spectral type. The effects of stellar evolution are again clearly seen, with stars moving horizontally to the right towards cooler temperatures as they evolve (assuming no mass loss). Note again that only the errors in \(T_{\rm eff}\) are large enough to be visible, while main-sequence masses for a given \(T_{\rm eff}\) may vary by 40% or more.