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We model the abundance gradients in the disk of the Milky Way for severalchemical elements (O, Mg, Si, S, Ca, Sc, Ti, Co, V, Fe, Ni, Zn, Cu, Mn, Cr, Ba,La and Eu), and compare our results with the most recent and homogeneousobservational data. We adopt a chemical evolution model able to well reproducethe main properties of the solar vicinity. We compute, for the first time, theabundance gradients for all the above mentioned elements in the galactocentricdistance range 4 - 22 kpc. The comparison with the observed data on Cepheids inthe galactocentric distance range 5-17 kpc gives a very good agreement for manyof the studied elements. In addition, we fit very well the data for theevolution of Lanthanum in the solar vicinity for which we present results herefor the first time. We explore, also for the first time, the behaviour of theabundance gradients at large galactocentric distances by comparing our resultswith data relative to distant open clusters and red giants and select the bestchemical evolution model model on the basis of that. We find a very good fit tothe observed abundance gradients, as traced by Cepheids, for most of theelements, thus confirming the validity of the inside-out scenario for theformation of the Milky Way disk as well as the adopted nucleosynthesisprescriptions.Comment: 11 pages, 9 figures, accepted for publication in A&

Abundance gradients in the Milky Way for α elements, iron peak elements, barium, lanthanum, and europium