  We numerically investigate the dynamical and chemical processes of the
formation of elliptical galaxies in a cold dark matter (CDM) universe, in order
to understand the origin of the mass-dependence of the photometric properties
of elliptical galaxies. Our three-dimensional TREE N-body/SPH numerical
simulations of elliptical galaxy formation take into account both Type II (SNe
II) and Type Ia (SNe Ia) supernovae (SNe) and follow the time evolution of the
abundances of several chemical elements (C, O, Ne, Mg, Si, and Fe). Moreover we
compare different strengths of SNe feedback.In combination with stellar
population synthesis, we derive the photometric properties of simulation
end-products, including the magnitude, color, half-light radius, and abundance
ratios, and compare them with the observed scaling relations directly and
quantitatively. We find that the extremely strong influence of SNe is required
to reproduce the observed color-magnitude relation (CMR), where we assume each
SN yields energy of 4x10^51 ergs and that 90% of this energy is ejected as
kinetic feedback. The feedback affects the evolution of lower mass systems more
strongly and induces the galactic wind by which a larger fraction of gas is
blown out in a lower mass system. Finally higher mass systems become more metal
rich and have redder colors than lower mass systems. We emphasize based on our
simulation results that the galactic wind is triggered mainly by SNe Ia rather
than SNe II. In addition we examined the Kormendy relation, which prescribes
the size of elliptical galaxies, and the [Mg/Fe]--magnitude relation, which
provides a strong constraint on the star formation history.
