  Motivated by the possible existence of other universes, this paper considers
the evolution of massive stars with different values for the fundamental
constants. We focus on variations in the triple alpha resonance energy and
study its effects on the resulting abundances of $^{12}$C, $^{16}$O, and larger
nuclei. In our universe, the $0^{+}$ energy level of carbon supports a resonant
nuclear reaction that dominates carbon synthesis in stellar cores and accounts
for the observed cosmic abundances. Here we define $\Delta{E}_R$ to be the
change in this resonant energy level, and show how different values affect the
cosmic abundances of the intermediate alpha elements. Using the state of the
art computational package $MESA$, we carry out stellar evolution calculations
for massive stars in the range $M_\ast$ = $15-40M_\odot$, and for a wide range
of resonance energies. We also include both solar and low metallicity initial
conditions. For negative $\Delta{E}_R$ , carbon yields are increased relative
to standard stellar models, and such universes remain viable as long as the
production of carbon nuclei remains energetically favorable, and stars remain
stable, down to $\Delta{E}_R\approx-300$ keV. For positive $\Delta{E}_R$,
carbon yields decrease, but significant abundances can be produced for
resonance energy increments up to $\Delta{E}_R\approx+500$ keV. Oxygen yields
tend to be anti-correlated with those of carbon, and the allowed range in
$\Delta{E}_R$ is somewhat smaller. We also present yields for neon, magnesium,
and silicon. With updated stellar evolution models and a more comprehensive
survey of parameter space, these results indicate that the range of viable
universes is larger than suggested by earlier studies.
