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dc.creatorMonroe, TalaWanda R.en_US
dc.creatorMelendez, Jorgeen_US
dc.creatorRamirez, Ivanen_US
dc.creatorYong, Daviden_US
dc.creatorBergemann, Mariaen_US
dc.creatorAsplund, Martinen_US
dc.creatorBedell, Meganen_US
dc.creatorMaia, Marcelo Tuccien_US
dc.creatorBean, Jacoben_US
dc.creatorLind, Karinen_US
dc.creatorAlves-Brito, Alanen_US
dc.creatorCasagrande, Lucaen_US
dc.creatorCastro, Matthieuen_US
dc.creatordo Nascimento, Jose-Diasen_US
dc.creatorBazot, Michaelen_US
dc.creatorFreitas, Fabricio C.en_US
dc.date.accessioned2016-10-28T19:38:48Z
dc.date.available2016-10-28T19:38:48Z
dc.date.issued2013-09en_US
dc.identifierdoi:10.15781/T2TT4FW48
dc.identifier.citationMonroe, TalaWanda R., Jorge Meléndez, Iván Ramírez, David Yong, Maria Bergemann, Martin Asplund, Megan Bedell et al. "High precision abundances of the old solar twin HIP 102152: insights on Li depletion from the oldest sun." The Astrophysical Journal Letters, Vol. 774, No. 2 (Sep., 2013): L32.en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/2152/43131
dc.description.abstractWe present the first detailed chemical abundance analysis of the old 8.2 Gyr solar twin, HIP 102152. We derive differential abundances of 21 elements relative to the Sun with precisions as high as 0.004 dex (<= 1%), using ultra high-resolution (R = 110,000), high S/N UVES spectra obtained on the 8.2 m Very Large Telescope. Our determined metallicity of HIP 102152 is [Fe/H] = -0.013 +/- 0.004. The atmospheric parameters of the star were determined to be 54 K cooler than the Sun, 0.09 dex lower in surface gravity, and a microturbulence identical to our derived solar value. Elemental abundance ratios examined versus dust condensation temperature reveal a solar abundance pattern for this star, in contrast to most solar twins. The abundance pattern of HIP 102152 appears to be the most similar to solar of any known solar twin. Abundances of the younger, 2.9 Gyr solar twin, 18 Sco, were also determined from UVES spectra to serve as a comparison for HIP 102152. The solar chemical pattern of HIP 102152 makes it a potential candidate to host terrestrial planets, which is reinforced by the lack of giant planets in its terrestrial planet region. The following non-local thermodynamic equilibrium Li abundances were obtained for HIP 102152, 18 Sco, and the Sun: log epsilon (Li) = 0.48 +/- 0.07, 1.62 +/- 0.02, and 1.07 +/- 0.02, respectively. The Li abundance of HIP 102152 is the lowest reported to date for a solar twin, and allows us to consider an emerging, tightly constrained Li-age trend for solar twin stars.en_US
dc.description.sponsorshipFAPESP 2010/19810-4, 2012/24392-2en_US
dc.description.sponsorshipNASAen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectplanetary systemsen_US
dc.subjectstars: abundancesen_US
dc.subjectsun: abundancesen_US
dc.subjectplanet Formationen_US
dc.subjectlithium abundancesen_US
dc.subjectchemical-compositionen_US
dc.subjectextrasolaren_US
dc.subjectplanetsen_US
dc.subjectparent starsen_US
dc.subject16 cygnien_US
dc.subjectsignatureen_US
dc.subjectevolutionen_US
dc.subjectrotationen_US
dc.subjectdwarfsen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleHigh Precision Abundances of the Old Solar Twin HIP 102152: Insights On Li Depletion from the Oldest Sunen_US
dc.typeArticleen_US
dc.description.departmentMcDonald Observatoryen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/2041-8205/774/2/l32en_US
dc.contributor.utaustinauthorRamirez, Ivanen_US
dc.relation.ispartofserialAstrophysical Journal Lettersen_US


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