Improved Laboratory Transition Probabilities for Nd II and Application to the Neodymium Abundances of the Sun and Three Metal-poor Stars

By E. A. Den Hartog, J. E. Lawler, C. Sneden, J. Cowan. 2003

188 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d3b9c26c07bb115d0eee567816dbe2102e65c26b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Timothy C. Beers
2. C. Sneden
3. Roberto Gallino
4. Martin Asplund
5. J. Cowan
6. Wak Aoki
7. N. Christlieb
8. A. Frebel

In Nuclear and High Energy Physics

1. C. Sneden
2. J. Cohen
3. Roberto Gallino
4. Jorge Meléndez
5. J. Cowan
6. Wak Aoki
7. Timothy C. Beers
8. J. E. Lawler

Citations in the corpus

• Abundances in a Large Sample of Stars in M3 and M13 (2004, methodology): “2004, AJ, 127, 1579 Brown, J. A., Wallerstein, G., & Oke, J. B. 1991, AJ, 101, 1693 Buonanno, R., Corsi, C. E., Buzzoni, A., Cacciari, C., Ferraro, F. R., & Fusi Pecci, F. 1994, A&A, 290, 69 Carretta, E., Bragaglia, A., & Cacciari, C. 2004a, ApJ, 610, L25 Carretta, E., Cohen, J. G., Gratton, R. G., ”
• 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, unknown): “…these ionized n-capture element species: Y, Hannaford et al. (1982); Zr, Malcheva et al. (2006); La, Lawler et al. (2001a); Ce, this study; 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. (2001c); Dy, Wickliffe et…”
• Neutron-Capture Elements in the Early Galaxy (2008, methodology): “5Cowan et al. (2002), with elemental updates provided by Den Hartog et al. (2003, 2005, 2006) and Lawler et al. (2004, 2006, 2007).”
• Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682) (2009, methodology): “The laboratory logg f published by Den Hartog et al. (2003) are very similar to the ones from VALD, except for the 5485 Å line, where they differ by 0.14 dex.”
• DETAILED CHEMICAL ABUNDANCES IN THE r-PROCESS-RICH ULTRA-FAINT DWARF GALAXY RETICULUM 2 (2016, methodology): “…Lawler et al. 2009; (22) Li et al. 2007, using HFS from Sneden et al. 2009; (23) Ivarsson et al. 2001, using HFS from Sneden et al. 2009; (24) Den Hartog et al. 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…”
• The Hamburg/ESO R-process enhanced star survey (HERES). II. Spectroscopic analysis of the survey sample (2005, methodology): “Neodymium We employ 9 lines of Nd II using laboratoryf - values from Den Hartog et al. (2003), which are a significant improvement on those previously available.”
• Spectroscopic Studies of Extremely Metal-Poor Stars with the Subaru High Dispersion Spectrograph. II. The r-Process Elements, Including Thorium (2004, methodology): “Studies of atomic data have progressed substantially lately, and therefore we can also make use of the newest data for Nd ii and Yb ii, reported by Den Hartog et al. (2003)andC.”
• Neutron-Capture Elements in the Very Metal Poor Star HD 122563 (2006, methodology): “— (1) Kurucz&Bell 1995; (2)Westin et al. 2000; (3) Lawler et al. 2001a; (4) Lawler et al. 2001b; (5) Johnson 2002; (6) Hill et al. 2002; (7) Cowan et al. 2002; (8) Sneden et al. 2003; (9) Den Hartog et al. 2003; (10) Johnson & Bolte 2004; (11) Lawler et al. 2004. based only on one or two lines, we e”
• Abundances In Very Metal-Poor Dwarf Stars (2004, methodology): “We have updated our Nd II gf values to those of Den Hartog et al. (2003).”
• A stellar census in globular clusters with MUSE: multiple populations chemistry in NGC 2808 (2019, methodology): “By comparing some of our synthetic spectra with the PHOENIX spectra, we realized that the updated atomic data for Fe I (Kurucz 2014) and Nd I (Den Hartog et al. 2003) retrieved from the VALD database (Ryabchikova et al. 2015) provided a better match and we updated the line lists accordingly.”
• The elemental composition of the Sun - III. The heavy elements Cu to Th (2014, methodology): “With the HM model, spectral synthesis and/or equivalent widths, and as many lines as possible, 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”
• The chemical composition of the Sun (2009, background): “…hyperfine constants for all the rare Earth elements: La (Lawler, Bonvallet & Sneden 2001), Ce (Lawler et 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.…”
• NEW RARE EARTH ELEMENT ABUNDANCE DISTRIBUTIONS FOR THE SUN AND FIVE r-PROCESS-RICH VERY METAL-POOR STARS (2009, background): “…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 al. (2007),…”
• The Hamburg/ESO R-process enhanced star survey (HERES) - III. HE 0338-3945 and the formation of the r + s stars (2006, methodology): “The oscillator strengths were taken from Den Hartog et al. (2003).”
• First stars VIII. Enrichment of the neutron-capture elements in the early Galaxy (2007, unknown): “The line list used to determine the heavy-element abundances is taken from Paper I, but updated with recent determinations of oscillator strengths and hyperfine structure corrections (Den Hartog et al. 2003; Lawler et al. 2004) for several of the elements.”