Elemental and isotopic abundances and chemical evolution of galaxies

Research output: Chapter in Book/Report/Conference proceedingConference contribution


Elemental 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.
Original languageEnglish
Title of host publicationVol. 458 The 3rd Subaru International Conference / The 1st NAOJ Symposium
EditorsWako Aoki
PublisherAstronomical Society of the Pacific
ISBN (Electronic)978-1-58381-799-5
ISBN (Print)978-1-58381-798-8
Publication statusPublished - 15 Feb 2012

Publication series

NameASP Conference Series Proceedings
PublisherAstronomical Society of the Pacific


  • astro-ph.GA
  • astro-ph.CO
  • astro-ph.SR


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