The Link Between Rare-Earth Peak Formation and the Astrophysical Site of the R Process

Mumpower, Matthew R.; McLaughlin, Gail C.; Surman, Rebecca; Steiner, Andrew W.

doi:10.3847/1538-4357/833/2/282

Title: The Link Between Rare-Earth Peak Formation and the Astrophysical Site of the R Process

Journal Article · Tue Dec 20 00:00:00 EST 2016 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/833/2/282· OSTI ID:1419745

^[1];

^[2]; Surman, Rebecca ^[3];

^[4]

Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Univ. of Notre Dame, IN (United States). Dept. of Physics
North Carolina State Univ., Raleigh, NC (United States). Dept. of Physics
Univ. of Notre Dame, IN (United States). Dept. of Physics
Univ. of Tennessee, Knoxville, TN (United States). Dept. of Physics and Astronomy; Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division

The primary astrophysical source of the rare-earth elements is the rapid neutron capture process (r process). The rare-earth peak that is seen in the solar r-process residuals has been proposed to originate as a pile-up of nuclei during the end of the r process. We introduce a new method utilizing Monte Carlo studies of nuclear masses in the rare-earth region, that includes self-consistently adjusting β-decay rates and neutron capture rates, to find the mass surfaces necessary for the formation of the rare-earth peak. We demonstrate our method with two types of astrophysical scenario, one corresponding to conditions typical of hot winds from core-collapse supernovae and stellar-mass accretion disks, and one corresponding to conditions typical of the ejection of the material from the tidal tails of neutron star mergers. In each type of astrophysical condition, this method successfully locates a region of enhanced stability in the mass surface that is responsible for the rare-earth peak. For each scenario, we find that the change in the mass surface has qualitatively different features, thus future measurements can shed light on the type of environment in which the r process occurred.

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Research Organization:: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States); Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)

Sponsoring Organization:: USDOE Office of Science (SC), Nuclear Physics (NP); USDOE National Nuclear Security Administration (NNSA); National Science Foundation (NSF)

Grant/Contract Number:: AC52-06NA25396; PHY1554876; PHY0822648; PHY1419765; SC0013039; FG02-02ER41216; AC05-00OR22725

OSTI ID:: 1419745

Alternate ID(s):: OSTI ID: 1460246

Report Number(s):: LA-UR-16-21461; TRN: US1801381

Journal Information:: The Astrophysical Journal (Online), Vol. 833, Issue 2; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 14 works

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