r-process Nucleosynthesis from Three-dimensional Magnetorotational Core-collapse Supernovae

Mösta, Philipp; Roberts, Luke F.; Halevi, Goni; Ott, Christian D.; Lippuner, Jonas; Haas, Roland; Schnetter, Erik

doi:10.3847/1538-4357/aad6ec

r-process Nucleosynthesis from Three-dimensional Magnetorotational Core-collapse Supernovae

Journal Article · Mon Sep 10 00:00:00 EDT 2018 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aad6ec· OSTI ID:1480039

^[1]; Roberts, Luke F. ^[2]; Halevi, Goni ^[3]; ^[4]; ^[5]; Haas, Roland ^[6]; ^[7]

Univ. of California, Berkeley, CA (United States)
Michigan State Univ., East Lansing, MI (United States)
Univ. of California, Berkeley, CA (United States); Princeton Univ., Princeton, NJ (United States)
California Inst. of Technology (CalTech), Pasadena, CA (United States); Kyoto Univ., Kyoto (Japan)
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Univ. of Illinois, Urbana-Champaign, IL (United States)
Perimeter Institute for Theoretical Physics, Waterloo, ON (Canada); Univ. of Guelph, Guelph, ON (Canada); Louisiana State Univ., Baton Rouge, LA (United States)

Here, we investigate r-process nucleosynthesis in 3D general-relativistic magnetohydrodynamic simulations of rapidly rotating strongly magnetized core collapse. The simulations include a microphysical finite-temperature equation of state and a leakage scheme that captures the overall energetics and lepton number exchange due to postbounce neutrino emission and absorption. We track the composition of the ejected material using the nuclear reaction network SkyNet. Our results show that the 3D dynamics of magnetorotational core-collapse supernovae (CCSN) are important for their nucleosynthetic signature. We find that production of r-process material beyond the second peak is reduced by a factor of 100 when the magnetorotational jets produced by the rapidly rotating core undergo a kink instability. Our results indicate that 3D magnetorotationally powered CCSNe are robust r-process sources only if they are obtained by the collapse of cores with unrealistically large precollapse magnetic fields of the order of 10¹³ G. Additionally, a comparison simulation that we restrict to axisymmetry results in overly optimistic r-process production for lower magnetic field strengths.

View Accepted Manuscript (DOE)

Research Organization:: Los Alamos National Laboratory (LANL)

Sponsoring Organization:: USDOE

Grant/Contract Number:: AC52-06NA25396

OSTI ID:: 1480039

Report Number(s):: LA-UR-17-31278

Journal Information:: The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 2 Vol. 864; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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