Improved Laboratory Transition Probabilities for Ce II, Application to the Cerium Abundances of the Sun and Five R-Process-Rich, Metal-Poor Stars, and Rare Earth Lab Data Summary

dc.contributor.utaustinauthorSneden, Christopheren_US
dc.creatorLawler, James E.en_US
dc.creatorSneden, Christopheren_US
dc.creatorCowan, John J.en_US
dc.creatorIvans,, Inese I.en_US
dc.creatorDen Hartog, E. A.en_US
dc.date.accessioned2016-10-28T19:34:01Z
dc.date.available2016-10-28T19:34:01Z
dc.date.issued2009-05en_US
dc.description.abstractRecent radiative lifetime measurements accurate to +/- 5% using laser-induced fluorescence (LIF) on 43 even-parity and 15 odd-parity levels of Ce II have been combined with new branching fractions measured using a Fourier transform spectrometer (FTS) to determine transition probabilities for 921 lines of Ce II. This improved laboratory data set has been used to determine a new solar photospheric Ce abundance, log epsilon = 1.61 +/- 0.01 (sigma = 0.06 from 45 lines), a value in excellent agreement with the recommended meteoritic abundance, log epsilon = 1.61 +/- 0.02. Revised Ce abundances have also been derived for the r-process-rich metal-poor giant stars BD+17 degrees 3248, CS 22892-052, CS 31082-001, HD 115444, and HD 221170. Between 26 and 40 lines were used for determining the Ce abundance in these five stars, yielding a small statistical uncertainty of +/- 0.01 dex similar to the solar result. The relative abundances in the metal-poor stars of Ce and Eu, a nearly pure r-process element in the Sun, matches r-process-only model predictions for solar system material. This consistent match with small scatter over a wide range of stellar metallicities lends support to these predictions of elemental fractions. A companion paper includes an interpretation of these new precision abundance results for Ce as well as new abundance results and interpretation for Pr, Dy, and Tm.en_US
dc.description.departmentMcDonald Observatoryen_US
dc.description.sponsorshipen_US
dc.identifierdoi:10.15781/T2WW7727X
dc.identifier.citationLawler, J. E., C. Sneden, J. J. Cowan, I. I. Ivans, and E. A. Den Hartog. "Improved Laboratory Transition Probabilities for Ce II, Application to the Cerium Abundances of the Sun and Five r-Process-Rich, Metal-Poor Stars, and Rare Earth Lab Data Summary." The Astrophysical Journal Supplement Series, Vol. 182, No. 1 (May, 2009): 51.en_US
dc.identifier.doi10.1088/0067-0049/182/1/51en_US
dc.identifier.issn0067-0049en_US
dc.identifier.urihttp://hdl.handle.net/2152/42906
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.relation.ispartofserialAstrophysical Journal Supplement Seriesen_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.rights.restrictionOpenen_US
dc.subjectatomic dataen_US
dc.subjectgalaxy: evolutionen_US
dc.subjectnuclear reactions, nucleosynthesis,en_US
dc.subjectabundancesen_US
dc.subjectstars: abundancesen_US
dc.subjectstars: individual (bd+17 degrees 3248, csen_US
dc.subject22892-052, cs 31082-001, hd 115444, hd 221170)en_US
dc.subjectstars: population iien_US
dc.subjectsun: abundancesen_US
dc.subjectargon branching ratiosen_US
dc.subjecttheoretical radiative lifetimesen_US
dc.subjectspectral-intensity calibrationen_US
dc.subjectneutron-capture elementsen_US
dc.subjectoscillator-strengthsen_US
dc.subjectchemical-compositionen_US
dc.subjectsolar abundanceen_US
dc.subjectastrophysical interesten_US
dc.subjecthigh-resolutionen_US
dc.subjectcs 31082-001en_US
dc.subjectastronomy & astrophysicsen_US
dc.titleImproved Laboratory Transition Probabilities for Ce II, Application to the Cerium Abundances of the Sun and Five R-Process-Rich, Metal-Poor Stars, and Rare Earth Lab Data Summaryen_US
dc.typeArticleen_US
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