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We investigate the time evolution and spatial variation of the stellarinitial mass function (IMF) in star-forming disk galaxies by usingchemodynamical simulations with an IMF model depending both on local densitiesand metallicities ([Fe/H]) of the interstellar medium (ISM). We find that theslope (alpha) of a power-law IMF (N(m) ~ m^-alpha) for stellar masses largerthan 1M_sun evolves from the canonical Salpeter IMF (alpha ~ 2.35) to bemoderately top-heavy one (alpha ~ 1.9) in the simulated disk galaxies withstarbursts triggered by galaxy interaction. We also find that alpha instar-forming regions correlates with star formation rate densities (Sigma_SFRin units of M_sun yr^{-1} kpc^{-2}). Feedback effects of Type Ia and IIsupernovae are found to prevent IMFs from being too top-heavy (alpha < 1.5).The simulation predicts alpha ~ 0.23 log Sigma_SFR + 1.7 for log Sigma_SFR > -2(i.e., more top-heavy in higher Sigma_SFR), which is reasonably consistent wellwith corresponding recent observational results. The present study alsopredicts that inner regions of starburst disk galaxies have smaller alpha thusare more top-heavy (d alpha/d R ~ 0.07 kpc^{-1} for R < 5 kpc). The predictedradial alpha gradient can be tested against future observational studies of thealpha variation in star-forming galaxies.

Evolution of the high-mass end of the stellar initial mass functions in starburst galaxies