2020
DOI: 10.1051/0004-6361/201937189
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A high-precision abundance analysis of the nuclear benchmark star HD 20

Abstract: Metal-poor stars with available detailed information about their chemical inventory pose powerful empirical benchmarks for nuclear astrophysics. Here we present our spectroscopic chemical abundance investigation of the metal-poor ([Fe/H] = −1.60 ± 0.03 dex), r-process-enriched ([Eu/Fe] = 0.73 ± 0.10 dex) halo star HD 20 using novel and archival high-resolution data at outstanding signalto-noise ratios (up to ∼ 1000 Å −1 ). By combining one of the first asteroseismic gravity measurements in the metal-poor regim… Show more

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Cited by 17 publications
(13 citation statements)
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“…Moreover, this star has extremely accurate stellar parameters (e.g. asteroseismic gravity, see Hanke et al 2020, for details), slight r-process enhancement, and the r-process contribution to each element has subsequently been filtered at an absolute level, log (X) + log (X r ), where the rfraction is taken from Table 5 in Hanke et al (2020). This enables a purer comparison to the r-process at a lower metallicity than the Sun.…”
Section: Discussionmentioning
confidence: 99%
“…Moreover, this star has extremely accurate stellar parameters (e.g. asteroseismic gravity, see Hanke et al 2020, for details), slight r-process enhancement, and the r-process contribution to each element has subsequently been filtered at an absolute level, log (X) + log (X r ), where the rfraction is taken from Table 5 in Hanke et al (2020). This enables a purer comparison to the r-process at a lower metallicity than the Sun.…”
Section: Discussionmentioning
confidence: 99%
“…Also shown are the solar s-and r-process contributions (Burris et al 2000) and the best-fit linear combination of the contributions. Finally, we overplot the r-process benchmark star HD 20 as black squares (Hanke et al 2020a).…”
Section: Fe-peak Elementsmentioning
confidence: 99%
“…We further ran the identical analyses as above using solar-scaled opacity distributions (ODFNEW) and take one-quarter of the ensuing deviation to mimic an ignorance of the α-enhancement in the star of 0.1 dex. The respective deviations of the abundance ratios from the bona fide results from the unaltered atmospheres are listed in Table 3; a conservative upper limit to the total systematic uncertainty in terms of the squared sum of all contributions is given in the last column, although strong correlations between the impacts from the various atmospheric parameters can be expected (see, e.g., McWilliam et al 1995;Hanke et al 2020a).…”
Section: Abundance Errorsmentioning
confidence: 99%
“…Finally, we refer to the recent analysis of the Galactic benchmark star HD20 using both UVES and MIKE spectra (Hanke et al 2020). Thanks to the very high S/N ratio of the spectra of this bright star (>400 for UVES and >1000 for MIKE), this comparison is adequate to highlight intrinsic differences solely due to the instruments (and not induced by the noise).…”
Section: Comparison Between Abundances From Uves and Mike Spectramentioning
confidence: 99%