Grids of stellar models with rotation IV. Models from 1.7 to 120 Msun at
  a metallicity Z = 0.0004
  The effects of rotation on stellar evolution are particularly important at
low metallicity, when mass loss by stellar winds diminishes and the surface
enrichment due to rotational mixing becomes relatively more pronounced than at
high metallicities. Here we investigate the impact of rotation and metallicity
on stellar evolution. Using a similar physics as in our previous large grids of
models at Z=0.002 and Z=0.014, we compute stellar evolution models with the
Geneva code for rotating and nonrotating stars with initial masses (Mini)
between 1.7 and 120 Msun and Z=0.0004 (1/35 solar). This is comparable to the
metallicities of the most metal poor galaxies observed so far, such as I Zw 18.
Concerning massive stars, both rotating and nonrotating models spend most of
their core-helium burning phase with an effective temperature higher than 8000
K. Stars become red supergiants only at the end of their lifetimes, and few
RSGs are expected. Our models predict very few to no classical Wolf-Rayet stars
as a results of weak stellar winds at low metallicity. The most massive stars
end their lifetimes as luminous blue supergiants or luminous blue variables, a
feature that is not predicted by models with higher metallicities.
Interestingly, due to the behavior of the intermediate convective zone, the
mass domain of stars producing pair-instability supernovae is smaller at
Z=0.0004 than at Z=0.002. We find that during the main sequence phase, the
ratio between nitrogen and carbon abundances (N/C) remains unchanged for
nonrotating models. However, N/C increases by factors of 10-20 in rotating
models at the end of the MS. Cepheids coming from stars with Mini > 4-6 Msun
are beyond the core helium burning phase and spend little time in the
instability strip. Since they would evolve towards cooler effective
temperatures, these Cepheids should show an increase of the pulsation period as
a function of age.
