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

Mösta, Philipp and Roberts, Luke F. and Halevi, Goni and Ott, Christian D. and Lippuner, Jonas and Haas, Roland and Schnetter, Erik (2018) r-process Nucleosynthesis from Three-dimensional Magnetorotational Core-collapse Supernovae. Astrophysical Journal, 864 (2). Art. No. 171. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20180926-131800822

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Abstract

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 10^(13) G. Additionally, a comparison simulation that we restrict to axisymmetry results in overly optimistic r-process production for lower magnetic field strengths.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aad6ecDOIArticle
ORCID:
AuthorORCID
Mösta, Philipp0000-0002-9371-1447
Roberts, Luke F.0000-0001-7364-7946
Ott, Christian D.0000-0003-4993-2055
Lippuner, Jonas0000-0002-5936-3485
Haas, Roland0000-0003-1424-6178
Schnetter, Erik0000-0002-4518-9017
Additional Information:© 2018 The American Astronomical Society. Received 2017 December 30; revised 2018 July 24; accepted 2018 July 24; published 2018 September 13. The authors would like to thank D. Kasen, E. Quataert, and D. Radice for discussions. This research was partially supported by NSF grants AST-1212170, CAREER PHY-1151197, OAC-1550514, and OCI-0905046. P.M. acknowledges support by NASA through Einstein Fellowship grant PF5-160140. This work was enabled in part by the NSF under Grant No. PHY-1430152 (JINA Center for the Evolution of the Elements). The simulations were carried out on XSEDE resources under allocation TG-AST160049 and on NSF/NCSA BlueWaters under NSF award PRAC OCI-0941653. This paper has been assigned Yukawa Institute for Theoretical Physics report number YITP-17-129 and LANL Report number LA-UR-17-31278. Software: Einstein Toolkit (Löffler et al. 2012; Mösta et al. 2014a), SkyNet (Lippuner & Roberts 2017), REACLIB (Cyburt et al. 2010), Matplotlib (Hunter 2007).
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFAST-1212170
NSFPHY-1151197
NSFOAC-1550514
NSFOCI-0905046
NASA Einstein FellowshipPF5-160140
NSFPHY-1430152
NSFOCI-0941653
Subject Keywords:gamma-ray burst: general – instabilities – magnetohydrodynamics (MHD) – neutrinos – nuclear reactions, nucleosynthesis, abundances – supernovae: general
Issue or Number:2
Record Number:CaltechAUTHORS:20180926-131800822
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180926-131800822
Official Citation:Philipp Mösta et al 2018 ApJ 864 171
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:89963
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:26 Sep 2018 21:36
Last Modified:09 Mar 2020 13:18

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