The calculations are performed with the Geneva stellar evolutionary code, whose
physical ingredients have been extensively described in the previous papers (see
for example Papers I and IV). In accordance with
those previous calculations, we apply a moderate overshooting for 
of
at the border of the convective core as defined by the
Schwarzschild criterion, where d is the overshooting
distance and 
the local pressure scale height.
The following improvements/modifications have been performed with respect to the previous grids in order to match the requirements for Z=0.1:
- The initial helium content is taken as Y=0.48. This follows from a
cosmological helium abundance of Y|Z=0=0.24 (Audouze 1987)
and a relative conservative value of the ratio of
helium to metal enrichment equal to 
. Other elemental
abundances are taken from the solar distribution scaled to the metallicity.
- The radiative opacities for the interior are taken from Iglesias & Rogers (1996), while the low-temperature opacities are taken from Alexander & Ferguson (1994). The latter account for a wide variety of atomic and molecular species.
- At Z=0.10, the criterion defining a star to be of the Wolf-Rayet type could be different from that at lower metallicities. However, in the absence of any observational counterpart of those objects at such high metallicities, we keep the same criterion as in Paper I, i.e. we consider that a star enters the WR stage when its surface hydrogen mass fraction becomes lower than 0.4 and its effective temperature is higher than 10000 K. The mass loss rates of these objects are then accordingly taken as in Paper I.
- The prescription for the mass loss rates at these high metallicities
is quite uncertain. For consistency with previous calculations performed at lower Z,
we keep the same prescription as in Paper I, with,
for all the non WR phases, a 
metallicity
dependence as indicated by stellar wind
models
(cf. Kudritzki et al. 1989),
according to which 
.
Given the large main sequence (MS) mass loss and especially the low initial
hydrogen content, very massive stars enter the WR phase rapidly during core
hydrogen burning. Following the WR mass loss prescription, this leads to the
ejection of almost the totality of the initial mass during the MS for M>
. These stars would probably end as white dwarfs.
Because of our total ignorance of the dependence of the mass
loss rate on stellar characteristics in such conditions, we do not present
evolutionary tracks for these stars.