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We analyze radial stellar metallicity and kinematic profiles out to 1Re in244 CALIFA galaxies ranging from morphological type E to Sd, to study theevolutionary mechanisms of stellar population gradients. We find that linearmetallicity gradients exhibit a clear correlation with galaxy morphologicaltype - with early type galaxies showing the steepest gradients. We show thatthe metallicity gradients simply reflect the local mass-metallicity relationwithin a galaxy. This suggests that the radial stellar population distributionwithin a galaxys effective radius is primarily a result of the \emph{in-situ}local star formation history. In this simple picture, the dynamically derivedstellar surface mass density gradient directly predicts the metallicitygradient of a galaxy. We show that this correlation and its scatter can bereproduced entirely by using independent empirical galaxy structural andchemical scaling relations. Using Schwarzschild dynamical models, we alsoexplore the link between a galaxys local stellar populations and their orbitalstructures. We find that galaxies angular momentum and metallicity gradientsshow no obvious causal link. This suggests that metallicity gradients in theinner disk are not strongly shaped by radial migration, which is confirmed bythe lack of correlation between the metallicity gradients and observable probesof radial migration in the galaxies, such as bars and spiral arms. Finally, wefind that galaxies with positive metallicity gradients become increasinglycommon towards low mass and late morphological types - consistent with stellarfeedback more efficiently modifying the baryon cycle in the central regions ofthese galaxies.

A dynamical view on stellar metallicity gradient diversity across the Hubble sequence with CALIFA