  We numerically investigate chemodynamical evolution of major disk-disk galaxy
mergers in order to explore the origin of mass-dependent chemical, photometric,
and spectroscopic properties observed in elliptical galaxies. We particularly
investigate the dependence of the fundamental properties on merger progenitor
disk mass (M_d). Main results obtained in this study are the following three.
(1) More massive (luminous) ellipticals formed by galaxy mergers between more
massive spirals have larger metallicity (Z) and thus show redder colors: The
typical metallicity ranges from ~ 1.0 solar abundance (Z~ 0.02) for ellipticals
formed by mergers with M_d = 10^10 M_solar to ~ 2.0 solar (Z ~ 0.04) for those
with M_d = 10^12 M_solar. (2) The absolute magnitude of negative metallicity
gradients developed in galaxy mergers is more likely to be larger for massive
ellipticals.
  Absolute magnitude of metallicity gradient correlates with that of age
gradient in ellipticals in the sense that an elliptical with steeper negative
metallicity gradient is more likely to show steeper age gradient. (3) Both
M/L_B and M/L_K, where M, L_B, and L_K are total stellar mass of galaxy
mergers, B-band luminosity, and K-band one, respectively, depend on galactic
mass in such a way that more massive ellipticals have larger M/L_B and smaller
M/L_K.
