Evolution of the high-mass end of the stellar initial mass functions in
  starburst galaxies
  We investigate the time evolution and spatial variation of the stellar
initial mass function (IMF) in star-forming disk galaxies by using
chemodynamical simulations with an IMF model depending both on local densities
and metallicities ([Fe/H]) of the interstellar medium (ISM). We find that the
slope (alpha) of a power-law IMF (N(m) ~ m^-alpha) for stellar masses larger
than 1M_sun evolves from the canonical Salpeter IMF (alpha ~ 2.35) to be
moderately top-heavy one (alpha ~ 1.9) in the simulated disk galaxies with
starbursts triggered by galaxy interaction. We also find that alpha in
star-forming regions correlates with star formation rate densities (Sigma_SFR
in units of M_sun yr^{-1} kpc^{-2}). Feedback effects of Type Ia and II
supernovae 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 well
with corresponding recent observational results. The present study also
predicts that inner regions of starburst disk galaxies have smaller alpha thus
are more top-heavy (d alpha/d R ~ 0.07 kpc^{-1} for R < 5 kpc). The predicted
radial alpha gradient can be tested against future observational studies of the
alpha variation in star-forming galaxies.
