  The Milky Way harbours two disks that appear distinct concerning
scale-heights, kinematics, and elemental abundance patterns. Recent years have
seen a surge of studies of the elemental abundance trends in the disks using
high resolution spectroscopy. Here I will review and discuss the currently
available data. Special focus will also be put on how we define stars to be
members of either disk, and how current models of galaxy formation favour that
thick disks are formed from several accreted bodies. The ability for the
stellar abundance trends to test such predictions are discussed.
