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

2009/03/11 by J. E. Lawler, C. Sneden, J. J. Cowan +2 · 152 citations
Physics and Astronomy · #Abundance (ecology) #Abundance of the chemical elements #Analytical Chemistry (journal) #Astronomy and Astrophysical Research #Cerium #Radiative transfer #Solar and Space Plasma Dynamics #Spectral line #Spectrometer #Stars #Stellar, planetary, and galactic studies #astro-ph.GA #astro-ph.SR

paper · pdf · doi:10.1088/0067-0049/182/1/51

published in The Astrophysical Journal Supplement Series 182(1), 51-79 (Institute of Physics) · 84 pages, 8 Figures, 14 Tables; To appear in the Astrophysical Journal Supplement

arxiv created 2009/03/11 · openalex publication_date 2009/04/15 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

Recent 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 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 interpretations for Pr, Dy and Tm.

Citations

• Neutron Capture in Low‐Mass Asymptotic Giant Branch Stars: Cross Sections and Abundance Signatures
• Table of nuclear magnetic dipole and electric quadrupole moments
• Solar System Abundances and Condensation Temperatures of the Elements
• On the possible presence of promethium in the spectra of HD 101065 (Przybylski's star) and HD 965

Cited by

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• Abundance Measurements of the Metal-poor M subdwarf LHS 174 Using High-resolution Optical Spectroscopy
• The elemental composition of the Sun
• Chemical abundances and kinematics of barium stars
• HEAVY-ELEMENT DISPERSION IN THE METAL-POOR GLOBULAR CLUSTER M92
• DETECTION OF ELEMENTS AT ALL THREEr-PROCESS PEAKS IN THE METAL-POOR STAR HD 160617,,

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