Quantum Monte Carlo calculation of the equation of state of neutron matter

Gandolfi, Stefano; Illarionov, A. Yu.; Schmidt, Kevin; Pederiva, Francesco; Fantoni, S.

doi:10.1103/physrevc.79.054005

Cited by 187 publications

(266 citation statements)

References 49 publications

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“…We simulated PNM with A = 66 and SNM with A = 28 nucleons in a periodic box, as described in [46] and [47]. The finite-size errors in PNM simulations have been investigated in [46] by comparing the Twist Averaged Boundary Conditions (TABC) with the Periodic Box Condition (PBC). It is remarkable that the energies of 66 neutrons computed using either twist averaging or periodic boundary conditions turn out to be almost the same.…”

Section: B Auxiliary Field Diffusion Monte Carlo (Afdmc) Approachmentioning

confidence: 99%

Density-dependent nucleon-nucleon interaction from three-nucleon forces

et al. 2011

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Microscopic calculations based on realistic nuclear hamiltonians, while yielding accurate results for the energies of the ground and low-lying excited states of nuclei with A ≤ 12, fail to reproduce the empirical equilibrium properties of nuclear matter, that are known to be significantly affected by three-nucleon forces. We discuss a scheme suitable to construct a density-dependent two-nucleon potential, in which the effects of n-particle interactions can be included by integrating out the degrees of freedom of (n − 2)-nucleons. Our approach, based on the formalism of correlated basis function and state-of-the-art models of the two-and three-nucleon potentials, leads to an effective interaction that can be easily employed in nuclear matter calculations, yielding results in good agreement with those obtained from the underlying three-body potential.

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Section: B Auxiliary Field Diffusion Monte Carlo (Afdmc) Approachmentioning

confidence: 99%

Density-dependent nucleon-nucleon interaction from three-nucleon forces

et al. 2011

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“…The BHF results are particularly insightful, because the total energy can be directly connected to the partial wave expansion and therefore to the microscopic properties of the in-medium NN interaction. We also compare, when possible, the BHF results with other many-body approaches [8,9], namely the Brueckner-BetheGoldstone (BBG) approach up to third order in the hole-line expansion [10], the self-consistent Green's function (SCGF) method [11][12][13], the auxiliary field diffusion Monte Carlo (AFDMC) [6], the Green's function Monte Carlo (GFMC) [5], and the Fermi hypernetted chain (FHNC) [14][15][16]. The comparisons should be helpful in quantifying theoretical uncertainties with respect to the EOS.…”

Section: Introductionmentioning

confidence: 99%

“…These potentials have been used in calculations of both finite nuclei [4] and infinite matter (see, e.g., Refs. [5] and [6]). A natural question then arises: How well can these truncated potentials replace the original V 18 ?…”

Section: Introductionmentioning

confidence: 99%

“…In particular, we use a family of simpler versions of the widely used Argonne V 18 potential [3]. The V 8 , V 6 , and V 4 potentials [4] are built by removing operatorial components of the interaction, while the remaining terms are readjusted (as indicated by the prime) to preserve as many lowest-order phase shifts and deuteron properties as possible. These potentials have been used in calculations of both finite nuclei [4] and infinite matter (see, e.g., Refs.…”

Section: Introductionmentioning

confidence: 99%

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Comparative study of neutron and nuclear matter with simplified Argonne nucleon-nucleon potentials

et al. 2012

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We present calculations of the energy per particle of pure neutron and symmetric nuclear matter with simplified Argonne nucleon-nucleon potentials for different many-body theories. We compare critically the BruecknerHartree-Fock results to other formalisms, such as the Brueckner-Bethe-Goldstone expansion up to third order, self-consistent Green's functions, auxiliary field diffusion Monte Carlo, and Fermi hypernetted chain. We evaluate the importance of spin-orbit and tensor correlations in the equation of state and find these to be important in a wide range of densities.

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“…The Urbana IX (UIX) three-body force has been originally proposed in combination with the Argonne AV18 and AV8' [12]. Although it slightly underbinds the energy of light nuclei, it has been extensively used to study the equation of state of nuclear and neutron matter [13][14][15]. In this paper we shall present a study of the neutron matter EOS based on different models of three-neutron forces giving specific values of the symmetry energy [15,16].…”

Section: Nuclear Hamiltonians and Quantum Monte Carlo Methodsmentioning

confidence: 99%

The EOS of Neutron Matter and the Effect of Λ Hyperons to Neutron Star Structure

Gandolfi

Lonardoni

2017

Proceedings of the 12th International Conference on Hypernuclear and Strange Particle Physics (HYP2015)

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The structure of neutron stars is determined by the equation of state of the matter inside the star, which relies on the knowledge of nuclear interactions. While radii of neutron stars mostly depend on the equation of state of neutron matter at nuclear densities, their maximum mass can be drastically affected by the appearance of hyperons at higher densities in the inner core of the star. We summarize recent quantum Monte Carlo results on the calculation of the equation of state of neutron matter at nuclear and higher densities. We report about the development of realistic hyperon-nucleon interactions based on the available experimental data for light-and medium-heavy hypernuclei and on the effect of Λ hyperons to the neutron star structure.

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Quantum Monte Carlo calculation of the equation of state of neutron matter

Cited by 187 publications

References 49 publications

Density-dependent nucleon-nucleon interaction from three-nucleon forces

Density-dependent nucleon-nucleon interaction from three-nucleon forces

Comparative study of neutron and nuclear matter with simplified Argonne nucleon-nucleon potentials

The EOS of Neutron Matter and the Effect of Λ Hyperons to Neutron Star Structure

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