  We present an extension of the set of models published in Limongi & Chieffi,
2018, ApJS, 237, 13, at metallicity two times solar, i.e. [Fe/H]=0.3. The key
physical properties of these models at the onset of the core collapse are
mainly due to the higher mass loss triggered by the higher metallicity: the
super solar metallicity (SSM) models reach the core collapse with smaller He-
and CO-core masses, while the amount of 12C left by the central He burning is
higher. These results are valid for all the rotation velocities. The yields of
the neutron capture nuclei expressed per unit mass of Oxygen (i.e. the X/O) are
higher in the SSM models than in the SM ones in the non rotating case while the
opposite occurs in the rotating models. The trend shown by the non rotating
models is the expected one, given the secondary nature of the n-capture
nucleosynthesis. Vice versa, the counter intuitive trend obtained in the
rotating models is the consequence of the higher mass loss present in the SSM
models that removes the H rich envelope faster than in the SM ones while the
stars are still in central He burning, dumping out the entanglement (activated
by the rotation instabilities) and therefore a conspicuous primary n-capture
nucleosynthesis.
