  We present detailed numerical calculations of the light element abundances
synthesized in a Universe consisting of matter- and antimatter- domains, as
predicted to arise in some electroweak baryogenesis scenarios. In our
simulations all relevant physical effects, such as baryon-antibaryon
annihilations, production of secondary particles during annihilations, baryon
diffusion, and hydrodynamic processes are coupled to the nuclear reaction
network. We identify two dominant effects, according to the typical spatial
dimensions of the domains. Small antimatter domains are dissipated via neutron
diffusion prior to He4 synthesis at T_He4 \approx 80 keV, leading to a
suppression of the primordial He4 mass fraction. Larger domains are dissipated
below T_He4 via a combination of proton diffusion and hydrodynamic expansion.
In this case the strongest effects on the elemental abundances are due to
anti-p He4 annihilations, leading to an overproduction of He3 relative to H2
and to overproduction of Li6 via non-thermal nuclear reactions. Both effects
may result in light element abundances deviating substantially from the
standard Big Bang Nucleosynthesis yields and from the observationally inferred
values. This allows us to derive stringent constraints on the antimatter
parameters. For some combinations of the parameters, one may obtain both, low
H2 and low He4, at a common value of the cosmic baryon density, a result
seemingly favored by current observational data.
