We first present chemodynamical simulations to investigate how stellar winds of
massive stars influence early dynamical and chemical evolution of forming globular clusters (GCs).
In our numerical models, GCs form in turbulent, high-density giant molecular clouds (GMCs),
which are embedded in a massive dark matter halo at high redshifts.
We show how high-density, compact stellar systems are formed from GMCs influenced both by physical processes
associated with star formation and by tidal fields of their host halos.
We also show that chemical pollution of GC-forming GMCs by stellar winds from massive stars
can result in star-to-star abundance inhomogeneities among light elements (e.g., C, N, and O) of stars
in GCs. The present model with a canonical initial mass function (IMF)
also shows a C-N anticorrelation that stars with smaller [C/Fe] have larger [N/Fe] in a GC.
Although these results imply that "self-pollution" of GC-forming GMCs by stellar winds from massive
stars can cause abundance inhomogeneities of GCs, the present models with different
parameters and canonical IMFs can not show N-rich stars with [N/Fe] ~ 0.8 observed in some GCs
(e.g., NGC 6752). We discuss this apparent failure in the context of massive star formation preceding
low-mass one within GC-forming GMCs ("bimodal star formation scenario").
We also show that although almost all stars (~97%) show normal He abundances (Y) of ~0.24
some stars later formed in GMCs can have Y as high as ~0.3 in some models.
The number fraction of He-rich stars with Y > 0.26 is however found to be small (~10-3) for most models.