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We present the first set of a new generation of models of massive stars ofsolar composition extending between 13 and 120 \msun, computed with and withoutthe effects of rotation. We included two instabilities induced by rotation,namely the meridional circulation and the shear instability. We implemented twoalternative schemes to treat the transport of the angular momentum: theadvection-diffusion formalism and the simpler purely diffusive one. The fullevolution from the Pre Main Sequence up to the presupernova stage is followedin detail with a very extended nuclear network. The explosive yields areprovided for a variety of possible mass cut and are available at the website\url{http://www.iasf-roma.inaf.it/orfeo/public{\_}html}.  We find that both the He and the CO core masses are larger than those oftheir non rotating counterparts. Also the C abundance left by the He burning islower than in the non rotating case, especially for stars of initial mass 13-25\msun, and this affects the final Mass-Radius relation, basically the finalbinding energy, at the presupernova stage. The elemental yields produced by ageneration of stars rotating initially at 300 km/s do not change substantiallywith respect to those produced by a generation of non rotating massive stars,the main differences being a slight overproduction of the weak s-component anda larger production of F. Since rotation also affects the mass loss rate,either directly and indirectly, we find substantial differences in thelifetimes as O-type and WR-subtypes between rotating and non rotating models.The maximum mass exploding as type IIP supernova ranges between 15 and 20\msunin both sets of models (this value depending basically on the larger mass lossrates in the Red Super Giant phase due to the inclusion of the dust drivenwind). This limiting value is in remarkable good agreement with currentestimates.

The evolution of rotating solar metallicity stars extending in mass from 13 to 120 msun: the hydrostatic evolution and the explosive yields