There are 4 files for each model:
mmmzvvv.cum_iso_nod     cumulative abundances starting from the surface
mmmzvvv.dif_iso_nod     abundances in mass fraction of all the isotopes in the network. unstable nuclei are allowed to decay only within the first 2.5e4 s from the explosion, then are kept freezed.
mmmzvvv.dif_iso_dec     abundances in mass fraction of all the isotopes in the network. all unstable nuclei are fully decayed.
mmmzvvvPRE.dif_iso_dec  preexplosive abundances in mass fraction of all the isotopes in the network. all unstable nuclei are fully decayed.

mmm is the mass
z the metallicity; a:solar
vvv the initial equatorial velocity

The first column in each file contains the mass coordinate (forget the second and the third columns), all others contain the mass fraction of each isotope. More specifically, consider rows j and j+1:
since the abundance of each isotope is assumed to be flat between two consecutive mass cordinates, the mass fractions x_j shown in row j represent the abundances of the isotopes between j and j+1.
