Disordered Nuclear Pasta, Magnetic Field Decay, and Crust Cooling in Neutron Stars

Horowitz, C. J.; Berry, Don; Briggs, Christian; Caplan, M. E.; Cumming, Andrew; Schneider, A.

doi:10.1103/physrevlett.114.031102

Cited by 162 publications

(147 citation statements)

References 30 publications

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“…[14] for a review of more recent works, including calculations of interest for corecollapse supernova. A recent investigation of the conductivity properties of the pasta phases has shown that topological defects affect the electrical conductivity of the system, originating a larger impurity parameter [15]. However, in Ref.…”

Section: Introductionmentioning

confidence: 99%

Effect of strong magnetic fields on the crust-core transition and inner crust of neutron stars

et al. 2017

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The Vlasov equation is used to determine the dispersion relation for the eigenmodes of magnetized nuclear and neutral stellar matter, taking into account the anomalous magnetic moment of nucleons. The formalism is applied to the determination of the dynamical spinodal section, a quantity that gives a good estimation of the crust-core transition in neutron stars. We study the effect of strong magnetic fields, of the order of 10 15 -10 17 G, on the extension of the crust of magnetized neutron stars. The dynamical instability region of neutron-proton-electron (npe) matter at subsaturation densities is determined within a relativistic mean-field model. It is shown that a strong magnetic field has a large effect on the instability region, defining the crust-core transition as a succession of stable and unstable regions due to the opening of new Landau levels. The effect of the anomalous magnetic moment is non-negligible for fields larger than 10 15 G. The complexity of the crust at the transition to the core and the increase of the crust thickness may have direct impact on the properties of neutrons stars related with the crust.

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Section: Introductionmentioning

confidence: 99%

Effect of strong magnetic fields on the crust-core transition and inner crust of neutron stars

et al. 2017

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“…This DiracBrueckner-Hartree-Fock (DBHF) approach (Brockmann and Machleidt, 1984;Horowitz and Serot, 1987;Ter Haar and Malfliet, 1987;Brockmann and Machleidt, 1990;Sammarruca, 2010) is computationally more involved than nonrelativistic BHF calculations and some ambiguities exist concerning the representation of the in-medium G matrix in terms of Lorentz invariants; see, e.g., the discussion by GrossBoelting, Fuchs, and Faessler (1999). However, the main advantage is that an additional repulsion at high densities is obtained since part of the three-body interaction is automatically generated (Brown, 1987).…”

Section: A Self-consistent Green's Functionmentioning

confidence: 99%

“…The Pauli exclusion principle can be incorporated approximately with appropriately designed contributions to the potentials. Central questions of MD calculations are the fragment recognition (Dorso and Randrup, 1993;Strachan and Dorso, 1997), the chemical composition (Horowitz, Berry, and Brown, 2007;Horowitz and Berry, 2009;Dorso, Giménez Molinelli, López, and Ramirez-Homs, 2012;, the appearance of different, sometimes complicated, shapes in the density distribution and their topological characterization (Watanabe et al, 2003b;Dorso, Giménez Molinelli, and López, 2012;Alcain, Giménez Molinelli, Nichols, and Dorso, 2014;Schneider et al, 2014;Horowitz et al, 2015), and phase transitions (Watanabe et al, 2005;. Structure functions and quantities related to the dynamical response can be extracted as well (Horowitz et al, , 2005Caballero et al, 2008;Berry, 2008, 2009).…”

Section: Nucleons-in-cell Calculationsmentioning

confidence: 99%

Equations of state for supernovae and compact stars

et al. 2017

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A review is given of various theoretical approaches for the equation of state (EoS) of dense matter, relevant for the description of core-collapse supernovae, compact stars, and compact star mergers. The emphasis is put on models that are applicable to all of these scenarios. Such EoS models have to cover large ranges in baryon number density, temperature, and isospin asymmetry. The characteristics of matter change dramatically within these ranges, from a mixture of nucleons, nuclei, and electrons to uniform, strongly interacting matter containing nucleons, and possibly other particles such as hyperons or quarks. As the development of an EoS requires joint efforts from many directions, different theoretical approaches are considered and relevant experimental and observational constraints which provide insights for future research are discussed. Finally, results from applications of the discussed EoS models are summarized.

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“…Horowitz et al suggest that topological defects in nuclear pasta increase electron-pasta scattering and reduce thermal conductivity [12]. They argue that this could slow crust cooling after accretion in low mass X-ray binaries.…”

Section: Introductionmentioning

confidence: 99%

Pasta nucleosynthesis: Molecular dynamics simulations of nuclear statistical equilibrium

et al. 2015

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Background Exotic non-spherical nuclear pasta shapes are expected in nuclear matter at just below saturation density because of competition between short range nuclear attraction and long range Coulomb repulsion.Purpose To explore the impact nuclear pasta may have on nucleosynthesis during neutron star mergers when cold dense nuclear matter is ejected and decompressed.Methods We use a hybrid CPU/GPU molecular dynamics (MD) code to perform decompression simulations of cold dense matter with 51 200 and 409 600 nucleons from 0.080 fm −3 down to 0.00125 fm −3 . Simulations are run for proton fractions YP = 0.05, 0.10, 0.20, 0.30, and 0.40 at temperatures T = 0.5, 0.75, and 1.0 MeV. The final composition of each simulation is obtained using a cluster algorithm and compared to a constant density run.Results Size of nuclei in the final state of decompression runs are in good agreement with nuclear statistical equilibrium (NSE) models for temperatures of 1 MeV while constant density runs produce nuclei smaller than the ones obtained with NSE. Our MD simulations produces unphysical results with large rod-like nuclei in the final state of T = 0.5 MeV runs.Conclusions Our MD model is valid at higher densities than simple nuclear statistical equilibrium models and may help determine the initial temperatures and proton fractions of matter ejected in mergers.

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Disordered Nuclear Pasta, Magnetic Field Decay, and Crust Cooling in Neutron Stars

Cited by 162 publications

References 30 publications

Effect of strong magnetic fields on the crust-core transition and inner crust of neutron stars

Effect of strong magnetic fields on the crust-core transition and inner crust of neutron stars

Equations of state for supernovae and compact stars

Pasta nucleosynthesis: Molecular dynamics simulations of nuclear statistical equilibrium

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