  We have re-studied line-strength gradients of 80 elliptical galaxies. Typical
metallicity gradients are d[Fe/H]/dlogr = -0.3. The metallicity gradients do
not correlate with any physical properties of galaxies, including central and
mean metallicities, central velocity dispersions sigma0, absolute B-magnitudes
MB, absolute effective radii Re, and dynamical masses of galaxies. By using the
metallicity gradients, we have calculated mean stellar metallicities for
individual ellipticals. Typical mean stellar metallicities are <[Fe/H]> = -0.3.
The mean metallicities correlate well with sigma0 and dynamical masses, though
relations for MB and Re include significant scatters. We find fundamental
planes defined by surface brightnesses SBe, <[Fe/H]>, and Re (or MB), and the
scatters of which are much smaller than those of the <[Fe/H]>-Re (or MB)
relations. The <[Fe/H]>-sigma0 relation is nearly in parallel to the [Fe/H]0-
sigma0 relation but systematically lower by 0.3 dex. The metallicity-mass
relation, or equivalently, the color-magnitude relation holds not only for the
central part but also for the whole part of galaxies. Using Mg2 and Fe1, we
find <[Mg/Fe]> = +0.2 in most of ellipticals. <[Mg/Fe]> shows no correlation
with galaxy mass tracers. This can be most naturally explained if the star
formation had stopped in ellipticals before the bulk of Type Ia supernovae
began to explode. Ellipticals can have significantly different metallicity
gradients and <[Fe/H]> even if they have the same galaxy mass. This may result
from galaxy mergers, but no evidence is found from presently available data to
support the same origin for metallicity gradients, the scatters around
metallicity-mass relation, and dynamical disturbances. This may suggest that
the scatters have their origin at the formation epoch of galaxies.
