Evolution of massive population III stars with rotation and magnetic fields

Context. Aims. We present a new grid of massive population III (Pop III) star models including the effects of rotation on the stellar structure and chemical mixing, and magnetic torques for the transport of angular momentum. This grid covers the range of mass from 10 to 1000 M, and rotational velocity from zero to 100 % of the critical rotation on the zero-age main sequence. Based on the grid, we also present a phase diagram for the expected final fates (i.e, core-collapse supernova, gamma-ray bursts and pair-instability supernovae of diverse types) of rotating massive Pop III stars. Methods. The model grid has been calculated with a stellar evolution code. We adopted the recent calibration made with the VLT-FLAMES data for the overshooting parameter and the chemical mixing efficiency due to rotation. The Spruit-Tayler dynamo was assumed for magnetic torques. Results. Our non-rotating models become redder than the previous models in the literature because of the larger overshooting pa-rameter adopted in this study. In particular, convective dredge-up of the helium core material into the hydrogen envelope is observed in our non-rotating very massive star models (∼> 200 M), which is potentially important for the chemical yields. On the other hand, the stars become bluer and more luminous with a higher rotational velocity. With the Spruit-Tayler dynamo, our models with a suffi-ciently high initial rotational velocity can reach the critical rotation earlier and lose more mass as a result, compared to the previou