All Tables

Table 1: Main physical inputs of the stellar models for the various initial masses considered. The labels "r'' and "s'' indicate respectively the models computed with or without rotation while the labels A-D refer to the choices in nuclear reactions (see text and Table 2). The initial value of $\Omega /\Omega _{\rm crit}$ is given. [I], [H02] and [H04] correspond respectively to Iliadis et al. (2001) and Hale et al. (2002,2004).
Table 2: Nuclear reaction rates adopted for the NeNa- and MgAl-chains in the sets B-D. [N], [I], [H02] and [H04] correspond respectively to Angulo et al. (1999), Iliadis et al. (2001) and Hale et al. (2002,2004). "Nom.'', "low.'' and "up.'' refer respectively to nominal, lower and upper limits of the experimental values. For all the other reactions of our network we use the NACRE nominal values.
Table 3: Initial abundances in mass fraction.
Table 4: Mean core abundance variations during MS of the 60 $M_\odot$ models. $\delta {\rm {X}}$ refers to the amplitude (in dex) of variation of element X. For NGC 6752 it refers to the amplitude variation observed between polluted and unpolluted stars.
Table 5: The main features of our models: initial mass, initial surface velocity, and for each evolutionary phase the remaining mass and the mean mass fraction in the wind for several isotopes integrated from the zero age main sequence. The 20, 40 and 120 $M_\odot$ models are computed with the reaction rates from set C. For rotating models the last division indicates abundance when He-burning products appear at the surface, or at the end of He-burning phase depending on the first case reached.