In the first paper of this series ( paper I ) we presented a new approach for studying the chemodynamical evolution in disk galaxies , focusing on the Milky Way .
While in paper I we studied extensively the Solar vicinity , here we extend these results to different distances from the Galactic center , looking for variations of observables that can be related to on-going and future spectroscopic surveys .
By separating the effects of kinematic heating and radial migration , we show that migration is much more important , even for the oldest and hottest stellar population .
The distributions of stellar birth guiding radii and final guiding radii ( signifying contamination from migration and heating , respectively ) widen with increasing distance from the Galactic center .
As a result , the slope in the age-metallicity relation flattens significantly at Galactic radii larger than solar .
We predict that the metallicity distributions of ( unbiased ) samples at different distances from the galactic center peak at approximately the same value , [ Fe/H ] \approx - 0.15 dex , and have similar metal-poor tails extending to [ Fe/H ] \approx - 1.3 dex .
In contrast , the metal-rich tail decreases with increasing radius , thus giving rise to the expected decline of mean metallicity with radius .
Similarly , the [ Mg/Fe ] distribution always peaks at \approx 0.15 dex , but its low-end tail is lost as radius increases , while the high-end tails off at [ Mg/Fe ] \approx 0.45 dex .
The radial metallicity and [ Mg/Fe ] gradients in our model show significant variations with height above the plane due to changes in the mixture of stellar ages .
An inversion in the radial metallicity gradient is found from negative to weakly positive ( at r < 10 kpc ) , and from positive to negative for the [ Mg/Fe ] gradient , with increasing distance from the disk plane .
We relate this to the combined effect of ( i ) the predominance of young stars close to the disk plane and old stars away from it , ( ii ) the more concentrated older stellar component , and ( iii ) the flaring of mono-age disk populations .
We also investigate the effect of recycled gas flows on the mean [ Fe/H ] and find that in the region 4 < r < 12 kpc the introduced errors are less than 0.05-0.1 dex , related to the fact that inward and outward flows mostly cancel in that radial range .
We show that radial migration can not compete with the inside-out formation of the disk , exposed by the more centrally concentrated older disk populations , and consistent with recent observations .