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dc.contributor.authorSuda, Takuma
dc.contributor.authorKomiya, Yutaka
dc.contributor.authorYamada, Shimako
dc.contributor.authorKatsuta, Yutaka
dc.contributor.authorAoki, Wako
dc.contributor.authorGil Pons, Pilar
dc.contributor.authorDoherty, Carolyn L.
dc.contributor.authorCampbell, Simon W.
dc.contributor.authorWood, Peter R.
dc.contributor.authorFujimoto, Masayuki Y.
dc.contributor.otherUniversitat Politècnica de Catalunya. Departament de Física Aplicada
dc.date.accessioned2014-03-31T11:59:46Z
dc.date.available2014-03-31T11:59:46Z
dc.date.created2013
dc.date.issued2013
dc.identifier.citationSuda, T. [et al.]. Transition of the stellar initial mass function explored using binary population synthesis. "Monthly notices of the Royal Astronomical Society", 2013, vol. 432, p. 46-50.
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/2117/22447
dc.description.abstractThe stellar initial mass function (IMF) plays a crucial role in determining the number of surviving stars in galaxies, the chemical composition of the interstellar medium, and the distribution of light in galaxies. A key unsolved question is whether the IMF is universal in time and space. Here we use state-of-the-art results of stellar evolution to show that the IMF of our Galaxy made a transition from an IMF dominated by massive stars to the present-day IMF at an early phase of the Galaxy formation. Updated results from stellar evolution in a wide range of metallicities have been implemented in a binary population synthesis code, and compared with the observations of carbon-enhanced metal-poor (CEMP) stars in our Galaxy. We find that applying the present-day IMF to Galactic halo stars causes serious contradictions with four observable quantities connected with the evolution of AGB stars. Furthermore, a comparison between our calculations and the observations of CEMP stars may help us to constrain the transition metallicity for the IMF which we tentatively set at [Fe/H] = -2. A novelty of the current study is the inclusion of mass loss suppression in intermediate-mass AGB stars at low-metallicity. This significantly reduces the overproduction of nitrogen-enhanced stars that was a major problem in using the high-mass star dominated IMF in previous studies. Our results also demonstrate that the use of the present day IMF for all time in chemical evolution models results in the overproduction of Type I.5 supernovae. More data on stellar abundances will help to understand how the IMF has changed and what caused such a transition.
dc.format.extent5 p.
dc.language.isoeng
dc.rightsAttribution-NonCommercial-NoDerivs 3.0 Spain
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/
dc.subjectÀrees temàtiques de la UPC::Aeronàutica i espai
dc.subject.lcshStars--Formation
dc.subject.lcshStars -- Evolution
dc.titleTransition of the stellar initial mass function explored using binary population synthesis
dc.typeArticle
dc.subject.lemacEstels -- Evolució
dc.contributor.groupUniversitat Politècnica de Catalunya. DF - Dinàmica No Lineal de Fluids
dc.identifier.doi10.1093/mnrasl/slt033
dc.description.peerreviewedPeer Reviewed
dc.rights.accessOpen Access
drac.iddocument12771513
dc.description.versionPreprint
upcommons.citation.authorSuda, T.; Komiya, Y.; Yamada, S.; Katsuta, Y.; Aoki, W.; Gil Pons, P.; Doherty, C. L.; Campbell, S.; Wood, P.; Fujimoto, M.
upcommons.citation.publishedtrue
upcommons.citation.publicationNameMonthly notices of the Royal Astronomical Society
upcommons.citation.volume432
upcommons.citation.startingPage46
upcommons.citation.endingPage50


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