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We explore the relations between physical and orbital properties of planetsand properties of their host stars to identify the main observable signaturesof the formation and evolution processes of planetary systems. We use a largesample of FGK dwarf planet hosts with stellar parameters derived in ahomogeneous way from the SWEET-Cat database to study the relation betweenstellar metallicity and position of planets in the period-mass diagram. In thesecond part we use all the RV-detected planets orbiting FGK stars to explorethe role of planet-disk and planet-planet interaction on the evolution oforbital properties of planets with masses above 1MJup. We show that planetsorbiting metal-poor stars have longer periods than those in metal-rich systems.This trend is valid for masses at least from 10MEarth to 4MJup. Earth-likeplanets orbiting metal-rich stars always show shorter periods (fewer than 20days) than those orbiting metal-poor stars. We also found statisticallysignificant evidence that very high mass giants have on average more eccentricorbits than giant planets with lower mass.Finally, we show that theeccentricity of planets with masses higher than 4MJup tends to be lower forplanets with shorter periods. Our results suggest that the planets in the P-MPdiagram are evolving differently because of a mechanism that operates over awide range of planetary masses. This mechanism is stronger or weaker dependingon the metallicity of the respective system. One possibility is that planets inmetal-poor disks form farther out from their central star and/or they formlater and do not have time to migrate as far as the planets in metal-richsystems. The trends and dependencies obtained for very high mass planetarysystems suggest that planet-disk interaction is a very important andorbit-shaping mechanism for planets in the high-mass domain. Shortened.

Orbital and physical properties of planets and their hosts: new insights on planet formation and evolution