Context :

Aims : We analyze chemical and kinematical properties of about 850 FGK solar neighborhood long-lived dwarfs observed with the HARPS high-resolution spectrograph .
The stars in the sample have \log g \geq 4 dex , 5000 \leq T { } _ { \mathrm { eff } } \leq 6500 K , and -1.39 \leq [ Fe/H ] \leq 0.55 dex .
The aim of this study is to characterize and explore the kinematics and chemical properties of stellar populations of the Galaxy in order to understand their origins and evolution .

Methods : We apply a purely chemical analysis approach based on the [ \alpha /Fe ] vs. [ Fe/H ] plot to separate Galactic stellar populations into the thin disk , thick disk and high- \alpha metal-rich ( h \alpha mr ) .
Then , we explore the population ’ s stellar orbital eccentricity distributions , their correlation with metallicity , and rotational velocity gradients with metallicity in the Galactic disks to provide constraints on the various formation models .

Results : We identified a gap in the [ \alpha /Fe ] - [ Fe/H ] plane for the \alpha -enhanced stars , and by performing a bootstrapped Monte Carlo test we obtained a probability higher than 99.99 % that this gap is not due to small-number statistics .
Our analysis shows a negative gradient of the rotational velocity of the thin disk stars with [ Fe/H ] ( -17 km s ^ { -1 } dex ^ { -1 } ) , and a steep positive gradient for both the thick disk and h \alpha mr stars with the same magnitude of about +42 km s ^ { -1 } dex ^ { -1 } .
For the thin disk stars we observed no correlation between orbital eccentricities and metallicity , but observed a steep negative gradient for the thick disk and h \alpha mr stars with practically the same magnitude ( \approx -0.18 dex ^ { -1 } ) .
The correlations observed for the nearby stars ( on average 45 pc ) using high-precision data in general agree well with the results obtained for the SDSS sample of stars located further from the Galactic plane .

Conclusions : Our results suggest that radial migration played an important role in the formation and evolution of the thin disk .
For the thick disk stars it is not possible to reach a firm conclusion about their origin .
Based on the eccentricity distribution of the thick disk stars only their accretion origin can be ruled out , and the heating and migration scenario could explain the positive steep gradient of V _ { \phi } with [ Fe/H ] .
Analyzing the h \alpha mr stellar population we found that they share properties of both the thin and thick disk population .
A comparison of the properties of the h \alpha mr stars with that of the subsample of stars from the N-body/SPH simulation using radial migration suggest that they may have originated from the inner Galaxy .
Further detailed investigations would help to clarify their exact nature and origin .