Show simple item record

dc.contributor.authorSouto, Diogo
dc.contributor.authorCunha, Katia
dc.contributor.authorSmith, Verne V.
dc.contributor.authorPrieto, C. Allende
dc.contributor.authorGarcía-Hernández, D. A.
dc.contributor.authorPinsonneault, Marc
dc.contributor.authorHolzer, Parker
dc.contributor.authorFrinchaboy, P. M.
dc.contributor.authorHoltzman, Jon
dc.contributor.authorJohnson, J. A.
dc.contributor.authorJönsson, Henrik
dc.contributor.authorMajewski, Steven R.
dc.contributor.authorShetrone, Matthew
dc.contributor.authorSobeck, Jennifer
dc.contributor.authorStringfellow, Guy
dc.contributor.authorTeske, Johanna
dc.contributor.authorZamora, Olga
dc.contributor.authorZasowski, Gail
dc.contributor.authorCarrera, Ricardo
dc.contributor.authorStassun, Keivan
dc.contributor.authorFernandez-Trincado, J. G.
dc.contributor.authorVillanova, Sandro
dc.contributor.authorMinniti, Dante
dc.contributor.authorSantana, Felipe
dc.date.accessioned2018-05-15T23:35:54Z
dc.date.available2018-05-15T23:35:54Z
dc.date.issued2018-04-10
dc.identifier.citationChemical Abundances of Main-sequence, Turnoff, Subgiant, and Red Giant Stars from APOGEE Spectra. I. Signatures of Diffusion in the Open Cluster M67 Diogo Souto, Katia Cunha, Verne V. Smith, et al. The Astrophysical Journal 857 (1) 14 (2018) DOI: 10.3847/1538-4357/aab612en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aab612
dc.identifier.urihttp://hdl.handle.net/10150/627626
dc.description.abstractDetailed chemical abundance distributions for 14 elements are derived for eight high-probability stellar members of the solar metallicity old open cluster M67 with an age of similar to 4 Gyr. The eight stars consist of four pairs, with each pair occupying a distinct phase of stellar evolution: two G dwarfs, two turnoff stars, two G subgiants, and two red clump (RC) K giants. The abundance analysis uses near-IR high-resolution spectra (lambda 1.5-1.7 mu m) from the Apache Point Observatory Galactic Evolution Experiment survey and derives abundances for C, N, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, and Fe. Our derived stellar parameters and metallicity for 2M08510076+1153115 suggest that this star is a solar twin, exhibiting abundance differences relative to the Sun of <= 0.04 dex for all elements. Chemical homogeneity is found within each class of stars (similar to 0.02 dex), while significant abundance variations (similar to 0.05-0.20 dex) are found across the different evolutionary phases; the turnoff stars typically have the lowest abundances, while the RCs tend to have the largest. Non-LTE corrections to the LTE-derived abundances are unlikely to explain the differences. A detailed comparison of the derived Fe, Mg, Si, and Ca abundances with recently published surface abundances from stellar models that include chemical diffusion provides a good match between the observed and predicted abundances as a function of stellar mass. Such agreement would indicate the detection of chemical diffusion processes in the stellar members of M67.en_US
dc.description.sponsorshipNational Aeronautics and Space Administration [16-XRP16_2-0004]; Ramon y Cajal fellowship [RYC-2013-14182]; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA-2014-58082-P]; National Science Foundation (NSF) [AST-1311835, AST-1715662]; Fondecyt [1170518]; Crafoord Foundation; Stiftelsen Olle Engkvist Byggmastare; Alfred P. Sloan Foundation; US Department of Energy Office of Science; Center for High-Performance Computing at the University of Utah; Brazilian Participation Group; Carnegie Institution for Science; Carnegie Mellon University; Chilean Participation Group; French Participation Group; Harvard-Smithsonian Center for Astrophysics; Instituto de Astrofisica de Canarias; Johns Hopkins University; Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo; Lawrence Berkeley National Laboratory; Leibniz Institut fur Astrophysik Potsdam (AIP); Max-Planck-Institut fur Astronomie (MPIA Heidelberg); Max-Planck-Institut fur Astrophysik (MPA Garching); Max-Planck-Institut fur Extraterrestrische Physik (MPE); National Astronomical Observatory of China; New Mexico State University; New York University; University of Notre Dame; Observatorio Nacional/MCTI; Ohio State University; Pennsylvania State University; Shanghai Astronomical Observatory; United Kingdom Participation Group; Universidad Nacional Autonoma de Mexico; University of Arizona; University of Colorado Boulder; University of Oxford; University of Portsmouth; University of Utah; University of Virginia; University of Washington; University of Wisconsin; Vanderbilt University; Yale Universityen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/857/i=1/a=14?key=crossref.a03d57c80887664b4ab3e43d88f117b4en_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.subjectdiffusionen_US
dc.subjectinfrared: starsen_US
dc.subjectopen clusters and associations: generalen_US
dc.subjectstars: abundancesen_US
dc.titleChemical Abundances of Main-sequence, Turnoff, Subgiant, and Red Giant Stars from APOGEE Spectra. I. Signatures of Diffusion in the Open Cluster M67en_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USAen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume857
dc.source.issue1
dc.source.beginpage14
refterms.dateFOA2018-05-15T23:35:55Z


Files in this item

Thumbnail
Name:
Souto_2018_ApJ_857_14.pdf
Size:
2.331Mb
Format:
PDF
Description:
Final Published Version

This item appears in the following Collection(s)

Show simple item record