Table 1: Comparison among evolutionary models for a star of 0.8 $M_{\odot }$ (Z=0.004 Y=0.238) by Girardi et al. (2000) and from the present work with different characteristics (see text). $\tau _{{\rm X}c=0}$and  $\tau _{\rm H_{shell}}$ represent the time (in Gyr) spent in the MS phase and in the SBG+RGB phases, respectively, while $\tau _{\rm L>1}$indicates the time in the RGB phase from log ( $L/L_{\odot })=1$ up to the He flash. Log  $L_{\rm ZAHB}$ is the luminosity of the ZAHB model for the 0.8 $M_{\odot }$ mass and  $\tau _{\rm HB}$ the time spent in the central He burning phase. The value of the R parameter is also shown.
  $\tau _{{\rm X}c=0}$ $\tau _{\rm H_{shell}}$ $\tau _{\rm L>1}$ $\log L_{\rm ZAHB}$ $\tau _{\rm HB}$ R

Girardi et al. (2000)

 15.881 2.273 0.243 1.665 0.123 1.89
No diffusion 14.504 3.093 0.278 1.771 0.086 1.46
Standard 13.853 3.067 0.289 1.754 0.084 1.33

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