Experimental Radiative Lifetimes, Branching Fractions, and Oscillator Strengths for La II and a New Determination of the Solar Lanthanum Abundance

By J. E. Lawler, G. Bonvallet, C. Sneden. 2001

278 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Mechanics of Materials, Statistics and Probability

View Paper: https://www.semanticscholar.org/paper/ad41d6cdcb6358f8d404fb46981dd85631d9e211

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Citations in the corpus

NEW RARE EARTH ELEMENT ABUNDANCE DISTRIBUTIONS FOR THE SUN AND FIVE r-PROCESS-RICH VERY METAL-POOR STARS (2009, unknown): “We have taken up the last consideration in the present series of papers: Lawler, Bonvallet, & Sneden (2001a), Lawler et al. (2001b), Lawler et al. (2001c), Den Hartog et al. (2003), Lawler, Sneden, & Cowan (2004), Den Hartog et al. (2005), Lawler et al. (2006), Den Hartog et al. (2006), Lawler et…”
Neutron-Capture Elements in the Very Metal Poor Star HD 122563 (2006, methodology): “In addition, the recent measurements of transition probabilities and hyperfine splitting reported for some elements (e.g., Lawler et al. 2001a, 2001b; Den Hartog et al. 2003) are incorporated.”
Probing the Neutron‐Capture Nucleosynthesis History of Galactic Matter (2002, background): “This survey employs higher resolution, higher S/N spectra and the new atomic data of Lawler et al. (2001).”
The Hamburg/ESO R-process enhanced star survey (HERES). II. Spectroscopic analysis of the survey sample (2005, methodology): “Oscillator strengths and hyperfine splitting from Lawler et al. (2001) were employed, assuming solar r-process isotopic fractions (supported by measurements by Sneden et al. 2002).”
Improved Laboratory Transition Parameters forEu II and Application to the Solar Europium Elemental and Isotopic Composition (2001, methodology): “These new data, in combination with recent work on La II (Lawler et al. 2001a), provide the basic spectroscopic data for much more accurate determinations of [Eu/La] in metal-poor halo stars.”
Abundances In Very Metal-Poor Dwarf Stars (2004, methodology): “We use the laboratory spectroscopy of Lawler, Bonvallet & Sneden (2001a) and Lawler et al. (2001b) to calculate the HFS patterns for La II and for Eu II.”
The elemental composition of the Sun - III. The heavy elements Cu to Th (2014, methodology): “…they have systematically applied their very accurate atomic data to the determination of the solar abundances of all the rare Earth elements (La: Lawler et al. 2001a, Ce: Lawler et al. 2009, Nd: Den Hartog et al. 2003, Sm: Lawler et al. 2006, Eu: Lawler et al. 2001b, Gd: Den Hartog et al. 2006,…”
Spectroscopic Studies of Very Metal-poor Stars with the Subaru High Dispersion Spectrograph. III. Light Neutron-Capture Elements (2005, methodology): “For the element Eu a spectrum synthesis technique was applied, because the three Eu ii lines analyzed in the present work show remarkably strong effects of hyperfine splitting (Lawler et al. 2001b).”
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, methodology): “Terbium is an on odd Z element with one stable isotope, 159Tb, with hfs from a nuclear spin I = 3/2 which is significant in stellar abundance work.”
HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS FROM SDSS/SEGUE. I. ATMOSPHERIC PARAMETERS AND CHEMICAL COMPOSITIONS (2012, unknown): “…(1980); (6)Ivans et al. (2006); (7)Lawler & Dakin (1989); (8)Blackwell et al. (1982a); (9)Blackwell et al. (1982b); (10)Pickering et al. (2001); (11)Ryabchikova et al. (1994); (12)Martin et al. (1988); (13)Booth et al. (1984); (14)O’Brian et al. (1991); (15) Schnabel et al. (2004); (16)Moity…”
Atomic Data for Resonance Absorption Lines. III. Wavelengths Longward of the Lyman Limit for the Elements Hydrogen to Gallium (2003, background): “Terbium (Tb), Z ¼ 65: Lawler et al. (2001a) have published A-values for Tb ii based on LIF lifetimes and FTS branching fractions.”
Improved Laboratory Transition Probabilities for Nd II and Application to the Neodymium Abundances of the Sun and Three Metal-poor Stars (2003, methodology): “We re-assessed the abundance of Eu for HD 115444 with the Eu ii line data of Lawler et al. (2001c), which were not available when this star was originally analyzed.”
DETAILED CHEMICAL ABUNDANCES IN THE r-PROCESS-RICH ULTRA-FAINT DWARF GALAXY RETICULUM 2 (2016, methodology): “…2003, using HFS/IS from Roederer et al. 2008a when available; (25) Lawler et al. 2006, using HFS/IS from Roederer et al. 2008a when available; (26) Lawler et al. 2001b, using HFS/IS from Ivans et al. 2006; (27) Den Hartog et al. 2006; (28) Lawler et al. 2001c, using HFS from Lawler et al. 2001d…”
Near-Ultraviolet Observations of HD 221170: New Insights into the Nature of r-Process-rich Stars (2006, methodology): “Modern transition probabilities based on a combination of radiative lifetimes from laser induced fluorescence (LIF) measurements and branching fractions from an FTS for the important strong lines of Eu ii and La ii were reported by Lawler et al. (2001a, 2001c).”
Spectroscopic Studies of Extremely Metal-Poor Stars with the Subaru High Dispersion Spectrograph. II. The r-Process Elements, Including Thorium (2004, methodology): “For La ii, Eu ii and Tb ii, we adopt the recent measurements of transition probabilities by Lawler et al. (2001a, 2001b, 2001c), respectively.”
“Sculptor-ing” the Galaxy? The Chemical Compositions of Red Giants in the Sculptor Dwarf Spheroidal Galaxy (2004, methodology): “…was included for the species Sc ii (with the hfs data taken from Prochaska & McWilliam 2000), Mn i (hfs data also taken from Prochaska & McWilliam 2000), Y i (with hfs data taken from Biehl 1976), La ii (with hfs data taken from Lawler et al. 2001), and Eu ii (with hfs data taken from Biehl 1976).”