All Tables

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.
Table 2: The V magnitude of the MS termination (MT), the difference in visual magnitude between the clump and MT ( $\Delta M_{V}$ ) and the clump mass (m in $M_{\odot }$ ) for the isochrones with age $\le$ 6 Gyr (see text) and chemical composition of LMC (Z=0.008 Y=0.25) are reported for the "standard'' (without overshooting) case and for the labelled assumptions on the overshooting parameter $\beta$ .
Table 3: As in Table 2 but for the metallicity of SMC (Z=0.004) and for the two studied values of the original helium abundance.
Table 4: The TO visual magnitudes, as a function of the age, for the studied chemical compositions.
Table 5: ZAHB visual magnitude in the RR Lyrae region ( $M_{V}^{\rm 3.83}$ ). The progenitor mass is 0.8 $M_{\odot }$ for Z=0.004 Y=0.27 and 0.9 $M_{\odot }$ in the other two cases.