  A sample of mostly old metal-rich dwarf and turn-off stars with high
eccentricity and low maximum height above the Galactic plane has been
identified. From their kinematics, it was suggested that the inner disk is
their most probable birthplace. Their chemical imprints may therefore reveal
important information about the formation and evolution of the still poorly
understood inner disk. To probe the formation history of these stellar
populations, a detailed analysis of a sample of very metal-rich stars is
carried out. We derive the metallicities, abundances of \alpha\ elements, ages,
and Galactic orbits. The analysis of 71 metal-rich stars is based on optical
high-resolution \'echelle spectra obtained with the FEROS spectrograph at the
ESO 1.52-m Telescope at La Silla, Chile. The metallicities and abundances of C,
O, Mg, Si, Ca, and Ti were derived based on LTE detailed analysis, employing
the MARCS model atmospheres. We confirm the high metallicity of these stars
reaching up to [Fe I/H]~0.58, and the sample of metal-rich dwarfs can be
kinematically subclassified in samples of thick disk, thin disk, and
intermediate stellar populations. All sample stars show solar \alpha-Fe ratios,
and most of them are old and still quite metal rich. The orbits suggest that
the thin disk, thick disk and intermediate populations were formed at
Galactocentric distances of ~8 kpc, ~6 kpc, and ~7 kpc, respectively. The mean
maximum height of the thick disk subsample of Z_max~380 pc, is lower than for
typical thick disk stars. A comparison of \alpha-element abundances of the
sample stars with bulge stars shows that the oxygen is compatible with a bulge
or inner thick disk origin. Our results suggest that models of radial mixing
and dynamical effects of the bar and bar/spiral arms might explain the presence
of these old metal-rich dwarf stars in the solar neighbourhood.
