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dc.contributor.authorKobayashi, Chiaki
dc.contributor.authorKarakas, Amanda I.
dc.contributor.authorUmeda, Hideyuki
dc.date.accessioned2011-12-20T13:01:05Z
dc.date.available2011-12-20T13:01:05Z
dc.date.issued2011-07
dc.identifier.citationKobayashi , C , Karakas , A I & Umeda , H 2011 , ' The evolution of isotope ratios in the Milky Way Galaxy ' , Monthly Notices of the Royal Astronomical Society , vol. 414 , no. 4 , pp. 3231-3250 . https://doi.org/10.1111/j.1365-2966.2011.18621.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 493407
dc.identifier.otherPURE UUID: 10fe51e4-a2a2-4970-873a-211b71df78aa
dc.identifier.otherWOS: 000293178600034
dc.identifier.otherScopus: 79959855794
dc.identifier.urihttp://hdl.handle.net/2299/7410
dc.description.abstractIsotope ratios have opened a new window into the study of the details of stellar evolution, supernovae and galactic chemical evolution. We present the evolution of the isotope ratios of elemental abundances (from C to Zn) in the solar neighbourhood, bulge, halo and thick disc, using chemical evolution models with updated yields of asymptotic giant branch (AGB) stars and core-collapse supernovae. The evolutionary history of each element is different owing to the effects of the initial progenitor mass and metallicity on element production. In the bulge and thick disc the star formation time-scale is shorter than in the solar neighbourhood, leading to higher [alpha/Fe] ratios. Likewise, the smaller contribution from Type Ia supernovae in these regions leads to lower [Mn/Fe] ratios. Also in the bulge, the abundances of [(Na, Al, P, Cl, K, Sc, Cu, Zn)/Fe] are higher because of the effect of metallicity on element production from core-collapse supernovae. According to our predictions, it is possible to find metal-rich stars ([Fe/H] greater than or similar to -1) that formed in the early Universe as a result of rapid star formation. The chemical enrichment time-scale of the halo is longer than in the solar neighbourhood, and consequently the ratios of [(C, F)/Fe] and C-12/C-13 are higher owing to a significant contribution from low-mass AGB stars. While the [alpha/Fe] and [Mn/Fe] ratios are the same as in the solar neighbourhood, the [(Na, Al, P, Cl, K, Sc, Cu, Zn)/Fe] ratios are predicted to be lower. Furthermore, we predict that isotope ratios such as Mg-24/Mg-25,Mg-26 are larger because of the contribution from low-metallicity supernovae. Using isotopic ratios, it is possible to select stars that formed in a system with a low chemical enrichment efficiency such as the satellite galaxies that were accreted on to our own Milky Way Galaxy.en
dc.format.extent20
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectstars: abundances
dc.subjectstars: AGB and post-AGB
dc.subjectsupernovae: general
dc.subjectGalaxy: abundances
dc.subjectGalaxy: evolution
dc.subjectASYMPTOTIC GIANT BRANCH
dc.subjectMETAL-POOR STARS
dc.subjectGALACTIC CHEMICAL EVOLUTION
dc.subjectINTERMEDIATE-MASS STARS
dc.subjectCORE-COLLAPSE SUPERNOVAE
dc.subjectHEAVY MAGNESIUM ISOTOPES
dc.subjectAGB STARS
dc.subjectFLUORINE ABUNDANCES
dc.subjectSOLAR NEIGHBORHOOD
dc.subjectGLOBULAR-CLUSTERS
dc.titleThe evolution of isotope ratios in the Milky Way Galaxyen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2011.18621.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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