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dc.contributor.authorKobayashi, Chiaki
dc.contributor.editorAoki, Wako
dc.date.accessioned2017-04-20T16:01:08Z
dc.date.available2017-04-20T16:01:08Z
dc.date.issued2012-02-15
dc.identifier.citationKobayashi , C 2012 , Elemental and isotopic abundances and chemical evolution of galaxies . in W Aoki (ed.) , Vol. 458 The 3rd Subaru International Conference / The 1st NAOJ Symposium . vol. 458 , ASP Conference Series Proceedings , Astronomical Society of the Pacific .en
dc.identifier.isbn978-1-58381-798-8
dc.identifier.isbn978-1-58381-799-5
dc.identifier.otherPURE: 11454908
dc.identifier.otherPURE UUID: c863520f-6421-4edd-b7d7-10d4357dcbae
dc.identifier.otherArXiv: http://arxiv.org/abs/1202.3356v1
dc.identifier.urihttp://hdl.handle.net/2299/18002
dc.identifier.urihttps://myasp.astrosociety.org/product/CS458/vol458the3rdsubaruinternationalconferencethe1stnaojsymposium.phpen
dc.descriptionChiaki Kobayashi, ‘Elemental and isotopic abundances and chemical evolution of galaxies’, paper presented at the 3rd Subaru International Conference: Galactic Archaeology, published as proceedings by the Astronomical Society of the Pacific, February 2012, ISBN 978-1-58381-798-8. Available online from the publisher at: https://myasp.astrosociety.org/product/CS458/vol458the3rdsubaruinternationalconferencethe1stnaojsymposium.php.en
dc.description.abstractElemental and isotopic abundances are the fossils of galactic archaeology. The observed [X/Fe]-[Fe/H] relations in the Galactic bulge and disk and the mass-metallicity relation of galaxies are roughly reproduced with chemodynamical simulations of galaxies under the standard \Lambda-CDM picture and standard stellar physics. The isotopic ratios such as ^{17,18}O and ^{25,26}Mg may require a refinement of modelling of supernova and asymptotic giant branch stars. The recent observation of the Carbon-rich damped Lyman \alpha system can be reproduced only with faint core-collapse supernovae. This suggests that chemical enrichment by the first stars in the first galaxies is driven not by pair-instability supernovae but by core-collapse supernovae (\sim 20-50M_\odot). The observed F abundances can be reproduced with the neutrino processes of core-collapse supernovae. As in F, the observations of elemental abundances in small systems may requires further complications of chemical enrichment. In globular clusters the relative contribution from low-mass supernovae is likely to be smaller than in the field, while the contribution from massive supernovae seems smaller in dwarf spheroidal galaxies than in the solar neighbourhood.en
dc.language.isoeng
dc.publisherAstronomical Society of the Pacific
dc.relation.ispartofVol. 458 The 3rd Subaru International Conference / The 1st NAOJ Symposiumen
dc.relation.ispartofseriesASP Conference Series Proceedingsen
dc.rightsen
dc.subjectastro-ph.GAen
dc.subjectastro-ph.COen
dc.subjectastro-ph.SRen
dc.titleElemental and isotopic abundances and chemical evolution of galaxiesen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematicsen
dc.contributor.institutionScience & Technology Research Instituteen
dc.contributor.institutionCentre for Astrophysics Researchen
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