Neutron-Capture Elements in the Very Metal Poor Star HD 122563

By Satoshi Honda, Wak Aoki, Y. Ishimaru, S. Wanajo, S. Ryan. 2006

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We obtained high-resolution, high signal-to-noise ratio (S/N) spectroscopy for the very metal poor star HD 122563 with the Subaru Telescope High Dispersion Spectrograph. Previous studies have shown that this object has excesses of light neutron-capture elements, while its abundances of heavy ones are very low. In our spectrum, which covers 3070-4780 Å of this object, 19 neutron-capture elements have been detected, including seven for the first time in this star (Nb, Mo, Ru, Pd, Ag, Pr, and Sm). Upper limits are given for five other elements including Th. The abundance pattern shows a gradually decreasing trend, as a function of atomic number, from Sr to Yb, which is quite different from those in stars with excesses of r-process elements. This abundance pattern of neutron-capture elements provides new strong constraints on the models of nucleosynthesis responsible for the very metal poor stars with excesses of light neutron-capture elements but without enhancement of heavy ones.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/79799495300ed84c43b36cf108f87ab11c977196

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Citations in the corpus

ELECTRON-CAPTURE SUPERNOVAE AS THE ORIGIN OF ELEMENTS BEYOND IRON (2010, methodology): “Spectroscopic studies of Galactic halo stars indicate the presence of a significant fraction of r-process deficient Galactic halo stars that possess high SrY-Zr (N = 50) abundances relative to heavy rprocess material (Johnson & Bolte 2002; Honda et al. 2006).”
CHARGED-PARTICLE AND NEUTRON-CAPTURE PROCESSES IN THE HIGH-ENTROPY WIND OF CORE-COLLAPSE SUPERNOVAE (2010, background): “…the full superposition of conditions required, is a matter of debate (see, e.g., Kratz et al. 1993; Wasserburg et al. 1996; Meyer & Brown 1997; Pfeiffer et al. 2001b; Sneden & Cowan 2003; Honda et al. 2006; Qian & Wasserburg 2007; Ott et al. 2008; Farouqi et al. 2009a, and references therein).”
Production of the entire range of r-process nuclides by black hole accretion disc outflows from neutron star mergers (2016, background): “11 shows the comparison of elemental abundances from three models (S-def, s6, s10) to the observed abundances in three metal-poor stars: CS22892-052 (Sneden et al. 2003), HD160617 (Roederer & Lawler 2012), and HD122563 (Honda et al. 2006, Roederer et al. 2012), normalized to the Eu abundance of CS22”
NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, background): “Two stars are typically identified with these trends: 1) CS 22829-052 (Sneden et al. 2003) and 2) HD 122563 (Wallerstein et al. 1963; Honda et al. 2004, 2006).”
Neutron-Capture Elements in the Early Galaxy (2008, background): “…(1963), that this brightest of all very metal-poor stars has some n-capture deficiencies but a large [Eu/Ba] value (the n-capture abundance pattern of HD 122563 was considered in more detail by Sneden & Parthasarathy 1983, and a comprehensive study has been published recently by Honda et al. 2006).”
Nucleosynthesis in the Early Galaxy (2007, background): “1 (Burris et al. 2000; Honda et al. 2004; Christlieb et al. 2004; Barklem et al. 2005; Honda et al. 2006).”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “They found that a somewhat lower Ye of ∼ 0.3 in the plumes might make ECSNe a site for a “weak r-process” that could explain the enhanced abundances of lighter r-process elements up to Ag and Pd in some metal-poor halo stars (Wanajo & Ishimaru 2006; Honda et al. 2006).”
THE ABUNDANCES OF NEUTRON-CAPTURE SPECIES IN THE VERY METAL-POOR GLOBULAR CLUSTER M15: A UNIFORM ANALYSIS OF RED GIANT BRANCH AND RED HORIZONTAL BRANCH STARS (2011, background): “Evidence of such a scenario (with multiple production pathways) may be also found in halo field stars of similar metallicity such as CS 22892-052 (Sneden et al. 2003(84)) and HD 122563 (Honda et al. 2006(47)), which have displayed similar abundance variations.”
HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS IN THE LEAST EVOLVED GALAXIES: URSA MAJOR II and COMA BERENICES (2009, background): “In Table 9, we list both our [X/Fe] abundances and those of the recent Aoki et al. (2007b) study (supplemented with neutron-capture abundances from Honda et al. 2006).”
On the astrophysical robustness of the neutron star merger r-process (2012, unknown): “Our findings of ejecta masses in the required range, extremely robust abundance patterns for the heaviest r-process elements, but underproduction of the lighter r-process elements, make compact binary mergers the major candidate for the observed, unique, heavy r-process component (Sneden et al. 2008”
Where, oh where has the r-process gone? (2007, methodology): “For the CPR nuclei, we obtain their H and L-yield patterns from the data on CS 22892–052 (Sneden et al., 2003) and HD 122563 (Honda et al., 2006).”
The s process: Nuclear physics, stellar models, and observations (2010, background): “The LEPP process is different from the s process in AGB stars and also different from the weak s-process component occurring in massive stars.”