  Massive stars blow powerful stellar winds throughout their evolutionary
stages from the main sequence to Wolf-Rayet phases. The amount of mechanical
energy deposited in the interstellar medium by the wind from a massive star can
be comparable to the explosion energy of a core-collapse supernova that
detonates at the end of its life. In this study, we estimate the kinetic energy
deposition by massive stars in our Galaxy by considering the integrated
Galactic initial mass function and modeling the stellar wind luminosity. The
mass loss rate and terminal velocity of stellar winds during the main sequence,
red supergiant, and Wolf-Rayet stages are estimated by adopting theoretical
calculations and observational data published in the literature. We find that
the total stellar wind luminosity due to all massive stars in the Galaxy is
about $L_w\approx 1.1\times 10^{41}$ erg/s, which is about 1/4 of the power of
supernova explosions, $L_{SN} \approx 4.8\times 10^{41}$ erg/s. If we assume
that $\sim 1-10$ % of the wind luminosity could be converted to Galactic cosmic
rays (GCRs) through collisonless shocks such as termination shocks in stellar
bubbles and superbubbles, colliding-wind shocks in binaries, and bow-shocks of
massive runaway stars, stellar winds might be expected to make a significant
contribution to GCR production, though lower than that of supernova remnants.
