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Domains and defects in nuclear pasta

Schneider, A. S. and Caplan, M. E. and Berry, D. K. and Horowitz, C. J. (2018) Domains and defects in nuclear pasta. Physical Review C, 98 (5). Art. No. 055801. ISSN 2469-9985. http://resolver.caltech.edu/CaltechAUTHORS:20180806-140329556

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Abstract

Nuclear pasta topology is an essential ingredient to determine transport properties in the inner crust of neutron stars. We perform semiclassical molecular dynamics simulations of nuclear pasta for proton fractions Y_p = 0.30 and Y_p = 0.40 near one-third of nuclear saturation density, n = 0.05fm^(−3), at a temperature T = 1.0MeV. Our simulations are, to our knowledge, the largest nuclear pasta simulations to date and contain up to 3276800 nucleons in the Y_p = 0.30 and 819200 nucleons in the Y_p = 0.40 case. An algorithm to determine which nucleons are part of a given sub-domain in the system is presented. By comparing runs of different sizes we study finite-size effects, equilibration time, the formation of multiple domains and defects in the pasta structures, as well as the structure factor dependence on simulation size. Although we find qualitative agreement between the topological structure and the structure factors of runs with 51 200 nucleons and those with 819200 nucleons or more, we show that simulations with hundreds of thousands of nucleons may be necessary to accurately predict pasta transport properties.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/PhysRevC.98.055801DOIArticle
https://arxiv.org/abs/1807.00102arXivDiscussion Paper
Additional Information:© 2018 American Physical Society. Received 2 July 2018; published 7 November 2018. We thank Greg Huber (KITP) and Kris Delaney (UCSB) for interesting and useful discussions regarding polymer topology and their similarities to nuclear pasta. We also thank William Newton (TAMU-Commerce) for sharing his insights on nuclear pasta domains, and Gerardo Ortiz (IU Bloomington) and Andrey Chugunov (IOFFE Institute St. Petersburg) for suggestions that helped improve this paper considerably. A.S.S. was supported in part by the Conselho Nacional de Desenvolvimento Científico e Tecnológico (201432/2014-5) and in part by the National Science Foundation under Award No. AST-1333520 and CAREER PHY-1151197. M.E.C. is supported by a fellowship from Canadian Institute for Theoretical Astrophysics. This research was supported in part by DOE Grants No. DE-FG02-87ER40365 (Indiana University) and No. DE-SC0018083 (NUCLEI SciDAC-4 Collaboration), and in part by Lilly Endowment, Inc., through its support for the Indiana University Pervasive Technology Institute, and in part by the Indiana METACyt Initiative. The Indiana METACyt Initiative at IU is also supported in part by Lilly Endowment, Inc. This research used resources of the Oak Ridge Leadership Computing Facility, which is a DOE Office of Science User Facility supported under Contract DE-AC05-00OR22725.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)201432/2014-5
NSFAST-1333520
NSFPHY-1151197
Canadian Institute for Theoretical AstrophysicsUNSPECIFIED
Department of Energy (DOE)DE-FG02-87ER40365
Department of Energy (DOE)DE-SC0018083
Lilly Endowment, Inc.UNSPECIFIED
Department of Energy (DOE)DE-AC05-00OR22725
Record Number:CaltechAUTHORS:20180806-140329556
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20180806-140329556
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:88614
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:06 Aug 2018 21:14
Last Modified:07 Nov 2018 17:42

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