Nucleosynthesis in the Early Galaxy

By F. Montes, Timothy C. Beers, J. Cowan, T. Elliot, K. Farouqi, Roberto Gallino, M. Heil, K. Kratz, B. Pfeiffer, M. Pignatari and 1 more. 2007

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Recent observations of r-process-enriched metal-poor star abundances reveal a nonuniform abundance pattern for elements Z ⩽ 47. Based on noncorrelation trends between elemental abundances as a function of Eu richness in a large sample of metal-poor stars, it is shown that the mixing of a consistent and robust light element primary process (LEPP) and the r-process pattern found in r-II metal-poor stars explains such apparent nonuniformity. Furthermore, we derive the abundance pattern of the LEPP from observation and show that it is consistent with a missing component in the solar abundances when using a recent s-process model. As the astrophysical site of the LEPP is not known, we explore the possibility of a neutron-capture process within a site-independent approach. It is suggested that scenarios with neutron densities nn ⩽ 1013 cm−3 or in the range nn ⩾ 1024 cm−3 best explain the observations.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/1211fcafe911b92a23c72b198015fa905105010d

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Citations in the corpus

Signatures of hypermassive neutron star lifetimes on r-process nucleosynthesis in the disc ejecta from neutron star mergers (2017, background): “06 21 6v 2 [ as tr o- poor stars show deviations from the solar system pattern relative to heavier elements (e.g., Montes et al. 2007).”
The s-Process in Massive Stars at Low Metallicity: The Effect of Primary 14N from Fast Rotating Stars (2008, background): “Another process must be responsible for the Sr observations, which is related to a similar observed Y and Zr overproduction with respect to Ba (e.g., Tr04, Montes et al. 2007).”
The s process: Nuclear physics, stellar models, and observations (2010, background): “Montes et al. (2007) surveyed the possible ranges of parameters (e.g. for the neutron density) that reproduce the abundance patterns of HD 122563, a very metal-poor star representing the yields of the LEPP (Honda et al., 2006).”
Neutrino-driven wind simulations and nucleosynthesis of heavy elements (2012, background): “Montes et al. (2007) [110] showed that there is an anticorrelation between heavy r-process and Sr-like elements in UMP stars.”
s-process production in rotating massive stars at solar and low metallicities (2015, background): “Later, Montes et al. (2007) compared the ‘stellar LEPP’ signature at low metallicity with the ‘solar LEPP’ in the Solar system, concluding that while they are compatible, also explosive nucleosynthesis processes can be responsible for the same elemental signature in the early Galaxy.”
Neutron-Capture Elements in the Early Galaxy (2008, background): “Refined calculations by Montes et al. (2007), attempting to reproduce the abundances of the r-process-poor star HD 122563 (Honda et al. 2006) and a sample of very metal-poor stars with various degrees of r-process enhancement, lend support to the existence of such a LEPP.”
THE s-PROCESS IN ASYMPTOTIC GIANT BRANCH STARS OF LOW METALLICITY AND THE COMPOSITION OF CARBON-ENHANCED METAL-POOR STARS (2011, background): “…in the initial s-process abundances may have arisen from pollution from primordial massive stars producing s-process elements during core He and shell C burning (Pignatari et al. 2008), or via the still unidentified “light element primary process” (Travaglio et al. 2004; Montes et al. 2007).”
Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, methodology): “In fact, this observable has been used as evidence of the existence of a LEPP10 to explain the abundance pattern of the elements in the atomic number range 38 < Z < 47 found in many halo stars (Travaglio et al. 2004; Montes et al. 2007; Qian & Wasserburg 2008; Arcones & Montes 2011).”
The long-term evolution of neutron star merger remnants – I. The impact of r-process nucleosynthesis (2013, unknown): “1 in Montes et al. (2007)).”