Two-dipole and three-dipole interaction coefficients of group XII elements

Shukla, Neelam; Kaur, Harpreet; Arora, Bindiya; Srivastava, Rajesh

doi:10.1016/j.physb.2021.413422

Cited by 2 publications

(2 citation statements)

References 62 publications

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“…We adopt the log(gf ) value for this line from Xu et al (2004), and its uncertainty is ≈0.05 dex. Recent theoretical calculations of the radiative lifetime of the 1 P 1 upper level (Yamaguchi et al 2019) and the oscillator strength (Shukla et al 2022) are in agreement with the Xu et al experimental value. The FIP of Cd is 8.99 eV, so a substantial fraction of neutral Cd is present in the atmosphere of HD 222925.…”

Section: A24 Ruthenium (Ru Z = 44)supporting

confidence: 84%

The R-Process Alliance: A Nearly Complete R-Process Abundance Template Derived from Ultraviolet Spectroscopy of the R-Process-Enhanced Metal-Poor Star HD 222925

Roederer,

Lawler,

Hartog

et al. 2022

Preprint

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We present a nearly complete rapid neutron-capture process (r-process) chemical inventory of the metal-poor ([Fe/H] = −1.46 ± 0.10) r-process-enhanced ([Eu/Fe] = +1.32 ± 0.08) halo star HD 222925. This abundance set is the most complete for any object beyond the solar system, with a total of 63 metals detected and seven with upper limits. It comprises 42 elements from 31 ≤ Z ≤ 90, including elements rarely detected in r-process-enhanced stars, such as Ga, Ge, As, Se, Cd, In, Sn, Sb, Te, W, Re, Os, Ir, Pt, and Au. We derive these abundances from an analysis of 404 absorption lines in ultraviolet spectra collected using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope and previously analyzed optical spectra. A series of appendices discusses the atomic data and quality of fits for these lines. The r-process elements from Ba to Pb, including all elements at the third r-process peak, exhibit remarkable agreement with the Solar r-process residuals, with a standard deviation of the differences of only 0.08 dex (17%). In contrast, deviations among the lighter elements from Ga to Te span nearly 1.4 dex, and they show distinct trends from Ga to Se, Nb through Cd, and In through Te. The r-process contribution to Ga, Ge, and As is small, and Se is the lightest element whose production is dominated by the r-process. The lanthanide fraction, log X La = −1.39±0.09, is typical for r-processenhanced stars and higher than that of the kilonova from the GW170817 neutron-star merger event. We advocate adopting this pattern as an alternative to the Solar r-process-element residuals when confronting future theoretical models of heavy-element nucleosynthesis with observations.

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Section: A24 Ruthenium (Ru Z = 44)supporting

confidence: 84%

The R-Process Alliance: A Nearly Complete R-Process Abundance Template Derived from Ultraviolet Spectroscopy of the R-Process-Enhanced Metal-Poor Star HD 222925

Roederer,

Lawler,

Hartog

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…We adopt the gf log( ) value for this line from Xu et al (2004), and its uncertainty is ≈0.05 dex. Recent theoretical calculations of the radiative lifetime of the 1 P 1 upper level (Yamaguchi et al 2019) and the oscillator strength (Shukla et al 2022) The relatively low Cd abundance in HD 222925 (Section 4.3) warrants additional scrutiny. Neglecting to model an unidentified blending feature would cause us to overestimate the Cd abundance, not underestimate it.…”

Section: A23 Molybdenum (Mo Z = 42)mentioning

confidence: 99%

The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925*

Roederer

Lawler

Hartog

et al. 2022

ApJS

View full text Add to dashboard Cite

We present a nearly complete rapid neutron-capture process (r-process) chemical inventory of the metal-poor ([Fe/H] = −1.46 ± 0.10) r-process-enhanced ([Eu/Fe] = +1.32 ± 0.08) halo star HD 222925. This abundance set is the most complete for any object beyond the solar system, with a total of 63 metals detected and seven with upper limits. It comprises 42 elements from 31 ≤ Z ≤ 90, including elements rarely detected in r-process-enhanced stars, such as Ga, Ge, As, Se, Cd, In, Sn, Sb, Te, W, Re, Os, Ir, Pt, and Au. We derive these abundances from an analysis of 404 absorption lines in ultraviolet spectra collected using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope and previously analyzed optical spectra. A series of appendices discusses the atomic data and quality of fits for these lines. The r-process elements from Ba to Pb, including all elements at the third r-process peak, exhibit remarkable agreement with the solar r-process residuals, with a standard deviation of the differences of only 0.08 dex (17%). In contrast, deviations among the lighter elements from Ga to Te span nearly 1.4 dex, and they show distinct trends from Ga to Se, Nb through Cd, and In through Te. The r-process contribution to Ga, Ge, and As is small, and Se is the lightest element whose production is dominated by the r-process. The lanthanide fraction, log X La = −1.39 ± 0.09, is typical for r-process-enhanced stars and higher than that of the kilonova from the GW170817 neutron-star merger event. We advocate adopting this pattern as an alternative to the solar r-process-element residuals when confronting future theoretical models of heavy-element nucleosynthesis with observations.

show abstract

Two-dipole and three-dipole interaction coefficients of group XII elements

Cited by 2 publications

References 62 publications

The R-Process Alliance: A Nearly Complete R-Process Abundance Template Derived from Ultraviolet Spectroscopy of the R-Process-Enhanced Metal-Poor Star HD 222925

The R-Process Alliance: A Nearly Complete R-Process Abundance Template Derived from Ultraviolet Spectroscopy of the R-Process-Enhanced Metal-Poor Star HD 222925

The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925*

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