J/A+A/679/A137ivo://CDS.VizieR/J/A+A/679/A137doi:10.26093/cds/vizier/bc-n7/lbdhCDSMartinet S.Meynet G.Ekstrom S.Georgy C.Hirschi R.2026-07-01T14:01:13Z2023-11-30T08:41:17ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frstellar-evolutionary-modelsstellar-masseschemical-abundancesIn addition to being spectacular objects, very massive stars (VMSs) are suspected to have a tremendous impact on their environment and on cosmic evolution in general. The nucleosynthesis both during their advanced stages and their final explosion may contribute greatly to the overall enrichment of the Universe. Their resulting supernovae are candidates for the most superluminous events possible and their extreme conditions also lead to very important radiative and mechanical feedback effects, from local to cosmic scale. We explore the impact of rotation and metallicity on the evolution of very massive stars across cosmic times. With the recent implementation of an equation of state in the GENEC stellar evolution code, appropriate for describing the conditions in the central regions of very massive stars in the advanced phases, we present new results on VMS evolution from Population III to solar metallicity. Low metallicity VMS models are highly sensitive to rotation, while the evolution of higher metallicity models is dominated by mass loss effects. The mass loss affects strongly their surface velocity evolution, breaking quickly at high metallicity while reaching the critical velocity for low metallicity models. The comparison to observed VMS in the LMC shows that the mass loss prescriptions used for these models are compatible with observed mass loss rates. In our framework for modelling rotation, our models of VMS need a high initial velocity to reproduce the observed surface velocities. The surface enrichment of these VMS is difficult to explain with only one initial composition, and could suggest multiple populations in the R136 cluster. At a metallicity typical of R136, only our non- or slowly rotating VMS models may produce Pair Instability supernovae. The most massive black holes that can be formed are less massive than about 60M_{sun}_. Direct observational constraints on VMS are still scarce. Future observational campaigns will hopefully gather more pieces of information to guide the theoretical modeling of these objects, whose impacts can be very important.2023A&A...679A.137Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/679/A137CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/679/A137https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/679/A137http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/679/A137https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/679/A137https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/679/A137http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/679/A137GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/679/A137/listList of model gridsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintZiniInitial metallicity Zphys.abund.ZcharMiniInitial mass modelphys.mass;meta.modelledcharRotRotating or non-rotating (Rot04 for V/Vc=0.4)meta.codecharFileNameName of the model grid in subdirectory tablesmeta.id;stat.param;meta.modelledchar