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Nuclear Pasta Formation

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arxiv 1307.1678 v1 pith:CYQTSH4N submitted 2013-07-05 nucl-th astro-ph.SR

classification nucl-thastro-ph.SR
keywords nuclearpastadensitydifferentmattersystemdecreasingenergy
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abstract

The formation of complex nonuniform phases of nuclear matter, known as nuclear pasta, is studied with molecular dynamics simulations containing 51200 nucleons. A phenomenological nuclear interaction is used that reproduces the saturation binding energy and density of nuclear matter. Systems are prepared at an initial density of 0.10fm$^{-3}$ and then the density is decreased by expanding the simulation volume at different rates to densities of 0.01 fm$^{-3}$ or less. An originally uniform system of nuclear matter is observed to form spherical bubbles ("swiss cheese"), hollow tubes, flat plates ("lasagna"), thin rods ("spaghetti") and, finally, nearly spherical nuclei with decreasing density. We explicitly observe nucleation mechanisms, with decreasing density, for these different pasta phase transitions. Topological quantities known as Minkowski functionals are obtained to characterize the pasta shapes. Different pasta shapes are observed depending on the expansion rate. This indicates non equilibrium effects. We use this to determine the best ways to obtain lower energy states of the pasta system from MD simulations and to place constrains on the equilibration time of the system.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. On variational trial functions in the extended Thomas-Fermi method

    nucl-th 2024-11 accept novelty 6.0 of 10

    A kink in the trial nucleon density at the center of cylindrical or plane-parallel Wigner-Seitz cells makes the fourth-order extended Thomas-Fermi energy divergent; only spherical-cell kinks are harmless.

  2. Constraints on Skyrme Equations of State from Doubly Magic Nuclei, Ab-Initio Calculations of Low-Density Neutron Matter, and Neutron Stars

    nucl-th 2019-08 conditional novelty 6.0 of 10

    The authors find that reproducing a 2.1 solar mass maximum neutron star requires a neutron effective mass of 0.60-0.65 at saturation density, leading to radius 12.4 km and tidal deformability 423 for a 1.4 solar mass star.

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