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Understanding the nature of the first stars is key to understanding the earlyuniverse. With new facilities such as JWST we may soon have the firstobservations of the earliest stellar populations, but to understand theseobservations we require detailed theoretical models. Here we compute a grid ofstellar evolution models using the Geneva code with the aim to improve ourunderstanding of the evolution of zero-metallicity stars, with particularinterest in how rotation affects surface properties, interior structure, andmetal enrichment. We produce a range of models of initial masses (Mini) from1.7 Msun to 120 Msun, focusing on massive models of 9 Msun < Mini < 120 Msun.Our grid includes models with and without rotation, with rotating models havingan initial velocity of 40% of the critical velocity. We find that rotationstrongly impacts the evolution of the first stars, mainly through increasedcore size and stronger H-burning shells during core He-burning. Withoutradiative mass loss, angular momentum builds at the surface in rotating models,thus models of initial masses Mini > 60 Msun reach critical rotation on themain sequence and experience mass loss. We find that rotational mixing stronglyaffects metal enrichment, but does not always increase metal production as wesee at higher metallicities. This is because rotation leads to an earlier CNOboost to the H shell during He-burning, which may hinder metal enrichmentdepending on initial mass and rotational velocity. Electronic tables of thisnew grid of Population III models are publicly available.

Grids of stellar models with rotation: V. Models from 1.7 to 120 Msun at zero metallicity