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dc.contributor.authorVincenzo, Fiorenzo
dc.contributor.authorMiglio, Andrea
dc.contributor.authorKobayashi, Chiaki
dc.contributor.authorMackereth, J. Ted
dc.contributor.authorMontalban, Josefina
dc.date.accessioned2019-08-07T17:36:45Z
dc.date.available2019-08-07T17:36:45Z
dc.date.issued2019-10-01
dc.identifier.citationVincenzo , F , Miglio , A , Kobayashi , C , Mackereth , J T & Montalban , J 2019 , ' He abundances in disc galaxies. I. Predictions from cosmological chemodynamical simulations ' , Astronomy & Astrophysics , vol. 630 , A125 . https://doi.org/10.1051/0004-6361/201935886
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 17171978
dc.identifier.otherPURE UUID: 9de9dc80-6644-4598-aa08-65a75598dfdd
dc.identifier.otherArXiv: http://arxiv.org/abs/1905.08309v2
dc.identifier.otherORCID: /0000-0002-4343-0487/work/62750469
dc.identifier.otherScopus: 85073233251
dc.identifier.urihttp://hdl.handle.net/2299/21586
dc.descriptionAccepted for publication in A&A
dc.description.abstractWe investigate how the stellar and gas-phase He abundances evolve as a function of time within simulated star-forming disc galaxies with different star formation histories. We make use of a cosmological chemodynamical simulation for galaxy formation and evolution, which includes star formation as well as energy and chemical enrichment feedback from asymptotic giant branch stars, core-collapse supernovae, and Type Ia supernovae. The predicted relations between the He mass fraction, Y, and the metallicity, Z, in the interstellar medium of our simulated disc galaxies depend on the galaxy star formation history. In particular, dY/dZ is not constant and evolves as a function of time, depending on the specific chemical element that we choose to trace Z; in particular, dY/dX O and dY/dX C increase as a function of time, whereas dY/dX N decreases. In the gas-phase, we find negative radial gradients of Y, due to the inside-out growth of our simulated galaxy discs as a function of time; this gives rise to longer chemical enrichment timescales in the outer galaxy regions, where we find lower average values for Y and Z. Finally, by means of chemical-evolution models, in the galactic bulge and inner disc, we predict steeper Y vs. age relations at high Z than in the outer galaxy regions. We conclude that for calibrating the assumed Y-Z relation in stellar models, C, N, and C+N are better proxies for the metallicity than O because they show steeper and less scattered relations.en
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.subjectastro-ph.GA
dc.subjectGalaxies: evolution
dc.subjectStars: abundances
dc.subjectISM: abundances
dc.subjectGalaxies: abundances
dc.subjectHydrodynamics
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleHe abundances in disc galaxies. I. Predictions from cosmological chemodynamical simulationsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85073233251&partnerID=8YFLogxK
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201935886
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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