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Matteo Cantiello edited sectionResultslabelresults.tex
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\section{Results}\label{results}
We calculated a grid of non-rotating stellar evolution sequences for initial masses
between $5\mso$ and $100\mso$, at metallicities of $Z$=0.02, $Z$=0.008 and $Z$=0.004, roughly corresponding to
the Galaxy, the LMC and the SMC, respectively. Additionally, we computed several models at
lower metallicity. Since rapid rotation can change the properties of
sub-surface convection \cite{Maeder2008}, we calculated a few rotating models to evaluate the effects of rotation on our results.
These effects are discussed in Section~\ref{rotation}.
Figures~\ref{fig:20zsunsurf} and~\ref{fig:60zsunsurf} show the evolution
of the radial extent and location of the sub-surface convection zones in
20$\mso$ and 60$\mso$ models during the main sequence phase.
