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The physics of stellar rotation plays a crucial role in the evolution ofstars, their final fate and the properties of compact remnants. Diverseapproaches have been adopted to incorporate the effects of rotation in stellarevolution models. This study seeks to explore the consequences of these variousprescriptions for rotation on essential outputs of massive star models. Wecompute a grid of 15 and 60 M$_{\odot}$ stellar evolution models with theGeneva Stellar Evolution Code (GENEC), accounting for both hydrodynamical andmagnetic instabilities induced by rotation. In both the 15 and 60 M$_{\odot}$models, the choice of the vertical and horizontal diffusion coefficients forthe non magnetic models strongly impacts the evolution of the chemicalstructure, but has a weak impact on the angular momentum transport and therotational velocity of the core. In the 15 M$_{\odot}$ models, the choice ofdiffusion coefficient impacts the convective core size during the coreH-burning phase, whether the model begins core He-burning as a blue or redsupergiant and the core mass at the end of He-burning. In the 60 M$_{\odot}$models, the evolution is dominated by mass loss and is less affected by thechoice of diffusion coefficient. In the magnetic models, magnetic instabilitydominates the angular momentum transport and such models are found to be lessmixed when compared to their rotating non-magnetic counterparts. Stellar modelswith the same initial mass, chemical composition, and rotation may exhibitdiverse characteristics depending on the physics applied. By conductingthorough comparisons with observational features, we can ascertain whichmethod(s) produce the most accurate results in different cases.

Impact of different approaches for computing rotating stellar models I. The solar metallicity case