Improved Laboratory Transition Parameters forEu II and Application to the Solar Europium Elemental and Isotopic Composition

By J. E. Lawler, M. Wickliffe, E. A. Den Hartog, C. Sneden. 2001

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Subfields: Astronomy and Astrophysics, Mechanics of Materials, Radiation

View Paper: https://www.semanticscholar.org/paper/faf82d8a4e4bb39d811f5112d5eac1e4327a14bb

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Citations in the corpus

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 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).”
The s process: Nuclear physics, stellar models, and observations (2010, background): “Thus, detailed analyses of Eu absorption line profiles enable one to estimate the Eu isotope ratios (Lawler et al., 2001).”
Abundances in giant stars of the globular cluster NGC 6752 (2005, unknown): “Certainly, the disagreement between our values and Norris & Da Costa (1995) for Nd and La is likely due to the different atomic data where we utilize the recently updated transition probabilities measured by Den Hartog et al. (2003) and Lawler et al. (2001a).”
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…”
alpha-, r-, and s-process element trends in the Galactic thin and thick disks (2004, methodology): “Linelists and logg f -values for the hyperfine components of the Eu lines have been kindly provided by C. Sneden and are the same as those used in the study by Lawler et al. (2001).”
S4N: A spectroscopic survey of stars in the solar neighborhood: The nearest 15 pc (2004, methodology): “In our favor we should stress that our analysis of this element benefits from the recent laboratory study of Eu II by Lawler et al. (2001) not available to most authors above.”
Solar Chemical Abundances Determined with a CO5BOLD 3D Model Atmosphere (2010, methodology): “Europium Basing our 3D LTE analysis (Mucciarelli et al., 2008) on the five Eu ii lines from Lawler et al. (2001), we obtain A(Eu)= 0.52 ± 0.02.”
Neutron-Capture Elements in the Early Galaxy (2008, result): “Their results are in excellent agreement with the precise Eu meteoritic ratio of f151 = 0.478 (e.g., Lodders 2003), as well as the Solar photospheric ratio 0.50 ± 0.07 (Hauge 1972, Lawler et al. 2001), deduced from the same transitions that are used for r-rich stars.”
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).”
CHEMICAL ABUNDANCES FOR 855 GIANTS IN THE GLOBULAR CLUSTER OMEGA CENTAURI (NGC 5139) (2010, methodology): “…determinations are more complicated than those for most elements because the line profiles are both affected by hyperfine splitting and Eu has two stable, naturally occurring isotopes (151Eu and 153Eu) with solar system isotopic fractions of 47.8% and 52.2%, respectively (Lawler et al. 2001b).”
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).”
First stars. I. The extreme r-element rich, iron-poor halo giant CS 31082-001 - Implications for the r-process site(s) and radioactive cosmochronology (2002, background): “Not that the europium hyperfine structure used here is from Kurucz (Kurucz 1993), although the oscillator strength was taken from the more recent work of Lawler et al. (2001b).”
The Rise of the s-Process in the Galaxy (2004, methodology): “This species has enjoyed a recent laboratory study that yielded accurate transition probabilities and hyperfine structure constants (Lawler et al. 2001a).”
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.”
The chemical composition of the Sun (2009, background): “…al. 2009), Pr (Sneden 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), Tb (Lawler et al. 2001a), Dy (Sneden et al. 2009), Ho (Lawler, Sneden & Cowan 2004), Er (Lawler et al. 2008), Tm, Yb and Lu (Sneden et al. 2009); the…”
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…”