  We investigate effects of triple-$\alpha$ and $^{12}\rm C(\alpha,\gamma)
^{16}O$ reaction rates on the production of supernova yields for a massive star
of 25 $M_{\odot}$. We combine the reaction rates to examine the rate
dependence, where the rates are considered to cover the possible variation of
the rates based on experiments on the earth and theories. We adopt four
combinations of the reaction rates from two triple-$\alpha$ reaction rates and
two $^{12}\rm C(\alpha,\gamma)^{16}O$ ones. First, we examine the evolution of
massive stars of 20 and 25 $M_{\odot}$ whose helium cores correspond to helium
stars of 6 and 8 $M_{\odot}$, respectively. While the 25 $M_{\odot}$ stars
evolve to the presupernova stages for all combinations of the reaction rates,
evolutionary paths of the 20 $M_{\odot}$ stars proceed significantly different
way for some combinations, which are unacceptable for progenitors of
supernovae. Second, we perform calculations of supernova explosions within the
limitation of spherical symmetry and compare the calculated abundance ratios
with the solar system abundances. We can deduce some constraints to the
reaction rates. As the results, a conventional rate is adequate for a
triple-$\alpha$ reaction rate and a rather higher value of the reaction rate
within the upper limit for the experimental uncertainties is favorable for a
$^{12}\rm C(\alpha,\gamma)^{16}O$ rate.
