  Employing the the stellar evolution code (Modules for Experiments in Stellar
Astrophysics), we calculate yields of heavy elements from massive stars via
stellar wind and core-collapse supernovae (CCSN) ejecta to interstellar medium
(ISM). In our models, the initial masses ($M_{\rm ini}$) of massive stars are
taken from 13 to 80 $M_\odot$, their initial rotational velocities (V) are 0,
300 and 500 km s$^{-1}$, and their metallicities are [Fe/H] = -3, -2, -1, and
0. The yields of heavy elements coming from stellar winds are mainly affected
by the stellar rotation which changes the chemical abundances of stellar
surfaces via chemically homogeneous evolution, and enhances mass-loss rate. We
estimate that the stellar wind can produce heavy element yields of about
$10^{-2}$ (for low metallicity models) to several $M_\odot$ (for low
metallicity and rapid rotation models) mass. The yields of heavy element
produced by CCSN ejecta also depend on the remnant mass of massive mass which
is mainly determined by the mass of CO-core. Our models calculate that the
yields of heavy elements produced by CCSN ejecta can get up to several
$M_\odot$. Compared with stellar wind, CCSN ejecta has a greater contribution
to the heavy elements in ISM. We also compare the $^{56}$Ni yields by
calculated in this work with observational estimate. Our models only explain
the $^{56}$Ni masses produced by faint SNe or normal SNe with progenitor mass
lower than about 25 $M_\odot$, and greatly underestimate the $^{56}$Ni masses
produced by stars with masses higher than about 30 $M_\odot$.
