Neutron-Capture Elements in the Early Galaxy

By C. Sneden, J. Cowan, Roberto Gallino. 2008

727 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/153932a4853d3c95fdd72fc4fbf060d4429e3ebc

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Citations in the corpus

• The Origin of r-process Elements in the Milky Way (2017, background): “…the hypothesis that GW170817 is a typical, representative event which produces a regular r-process signature, consistent with the robust abundance pattern observed in metal-poor halo stars (Sneden et al. 2008) and the ultra-faint dwarf galaxy Reticulum II (Ji et al. 2016; Roederer et al. 2016).”
• s‐Process in low‐metallicity stars – I. Theoretical predictions (2010, background): “The differences between models presented here and previous publications (Bisterzo et al. 2009; Sneden et al. 2008) are principally due to the correction of a past bug in the code, where we did not account for the poisoning effect of 16O in the pocket produced by the 13C(α, n)16O reaction.”
• The s-Process in Massive Stars at Low Metallicity: The Effect of Primary 14N from Fast Rotating Stars (2008, background): “In particular, the r−process is responsible for the production of about 20 % of solar Ba and 12 % of solar Sr, causing a [Sr/Ba]r = −0.22 (Sneden et al. 2008).”
• THE s-PROCESS IN ASYMPTOTIC GIANT BRANCH STARS OF LOW METALLICITY AND THE COMPOSITION OF CARBON-ENHANCED METAL-POOR STARS (2011, methodology): “Following on from the discovery of a large number of halo stars with peculiar chemical compositions the last decade has seen much interest sparked in detailed spectroscopic observations and nucleosynthetic models of stars of low metallicity (Beers & Christlieb 2005; Sneden et al. 2008).”
• Kilonova from post-merger ejecta as an optical and near-infrared counterpart of GW170817 (2017, unknown): “It is known that abundances of r-process elements in Galactic stars show an universal pattern similar to those of the Sun (e.g., Sneden et al. 2008), which implies that a certain phenomenon produces a wide range of r-process elements simultaneously.”
• Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “12, where we display the solar system s-fraction of the heavy elements (red circles; Sneden et al. 2008) and the corresponding values of our model (black squares).”
• Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, background): “…to a rare, robust event (such as a NSM) as the main "strong" r-process producer: the robust pattern of abundances in oldmetal-poor r-process stars (Sneden et al. 2008), the absence of any traces of recent 244Pu in deep sea reservoirs (Turner et al. 2004; Wallner et al. 2015; Hotokezaka et al.…”
• OPACITIES AND SPECTRA OF THE r-PROCESS EJECTA FROM NEUTRON STAR MERGERS (2013, background): “In principle, analysis of the light curves and spectra of these radioactive transients could be used to quantify the mass and chemical composition of the ejecta, which would clarify the unknown site(s) of r-process nucleosynthesis (e.g., Arnould et al. 2007; Sneden et al. 2008).”
• THE MOST METAL-POOR STARS. IV. THE TWO POPULATIONS WITH [Fe/H] ≲ −3.0 (2012, background): “For example, since the discovery and analysis of the highly r-process-element enhanced star CS 22892–052 (McWilliam et al. 1995; Sneden et al. 1996), several additional examples of this class have been identifid (see Sneden et al. 2008 and references therein).”
• The two metallicity groups of the globular cluster M 22: a chemical perspective (2011, background): “This suggested link between n-capture-rich stars in M22 with the s-process is sensible but not definitive, because Y, Zr, Ba also can be synthesized in the r-process (e.g, see the review by Sneden et al. 2008, which has references to individual r-process-rich stars).”
• DETAILED CHEMICAL ABUNDANCES IN THE r-PROCESS-RICH ULTRA-FAINT DWARF GALAXY RETICULUM 2 (2016, unknown): “Nd, Sm, and Eu (Sneden et al. 2008).”
• The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, methodology): “This is also the metallicity at which CEMP stars with s-process elements become more common, compared to the CEMP stars without neutron-capture element overabundances, which dominate at lower metallicities (Beers & Christlieb 2005; Sneden et al. 2008; Frebel & Norris 2013).”
• SYSTEMATICS OF DYNAMICAL MASS EJECTION, NUCLEOSYNTHESIS, AND RADIOACTIVELY POWERED ELECTROMAGNETIC SIGNALS FROM NEUTRON-STAR MERGERS (2013, background): “…a simple comparison of the observed abundance ratio with the production ratio can provide an age estimate of the contaminated object (Butcher 1987; Francois et al. 1993; Cowan et al. 1999; Goriely & Clerbaux 1999; Goriely & Arnould 2001; Cayrel et al. 2001; Frebel et al. 2007; Sneden et al. 2008).”
• CARBON-ENHANCED METAL-POOR STARS IN SDSS/SEGUE. I. CARBON ABUNDANCE ESTIMATION AND FREQUENCY OF CEMP STARS (2013, unknown): “…asymptotic giant 15 [C/Fe]=log10(N(C) /N(Fe))⋆ – log10(N(C)/N(Fe))⊙ branch (AGB) star to its (presently observed) binary companion (e.g., Herwig 2005; Sneden et al. 2008; Masseron et al. 2010; Bisterzo et al. 2011, 2012); (2) massive, rapidly rotating, zero-metallicity stars, which produce large…”