Improved variational calculations of nucleon matter

Morales, J. R.; Pandharipande, V.R.; Ravenhall, D. G.

doi:10.1103/physrevc.66.054308

Cited by 59 publications

(61 citation statements)

References 25 publications

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“…The stars in this figure give results of the recent variational calculations [27] with the full Argonne v18 and Urbana IX interactions. At low densities the two-body v CB is not a bad approximation; however, the E 0 (ρ) obtained from it does not show a minimum at ρ 0 .…”

Section: Correlated Basis Interactionmentioning

confidence: 99%

Quenching of weak interactions in nucleon matter

Cowell

Pandharipande

2003

Phys. Rev. C

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We have calculated the one-body Fermi and Gamow-Teller charge-current, and vector and axialvector neutral-current nuclear matrix elements in nucleon matter at densities of 0.08, 0.16 and 0.24 fm −3 and proton fractions ranging from 0.2 to 0.5. The correlated states for nucleon matter are obtained by operating on Fermi-gas states by a symmetrized product of pair correlation operators determined from variational calculations with the Argonne v18 and Urbana IX two-and threenucleon interactions. The squares of the charge current matrix elements are found to be quenched by 20 to 25 % by the short-range correlations in nucleon matter. Most of the quenching is due to spin-isospin correlations induced by the pion exchange interactions which change the isospins and spins of the nucleons. A large part of it can be related to the probability for a spin up proton quasi-particle to be a bare spin up/down proton/neutron. Within the interval considered the charge current matrix elements do not have significant dependence on the matter density, proton fraction and magnitudes of nucleon momenta; however, they do depend upon momentum transfer.The neutral current matrix elements have a significant dependence on the proton fraction. We also calculate the matrix elements of the nuclear Hamiltonian in the same correlated basis. These provide relatively mild effective interactions which give the variational energies in the HartreeFock approximation. The calculated two-nucleon effective interaction describes the spin-isospin susceptibilities of nuclear and neutron matter fairly accurately. However ≥ 3-body terms are necessary to reproduce the compressibility. Realistic calculations of weak interaction rates in nucleon matter can presumably be carried out using the effective operators and interactions studied here. All presented results use the simple 2-body cluster approximation to calculate the correlated basis matrix elements. This allows for a clear discussion of the physical effects in the effective operators and interactions.

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Section: Correlated Basis Interactionmentioning

confidence: 99%

Quenching of weak interactions in nucleon matter

Cowell

Pandharipande

2003

Phys. Rev. C

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“…One approach relies on determining the two-body potentials in the vicinity of ρ s using nucleon-nucleon scattering data below 350 MeV and the properties of light nuclei, in addition to incorporating the contributions from the three-body potentials (Akmal, Pandharipande, & Ravenhall 1998;Morales, Pandharipande, Ravenhall 2002;Gandolfi, Carlson, & Reddy 2012). The expansion in terms of many body interactions, however, breaks down at densities larger than ρ s .…”

Section: Neutron Star Structure and Equation Of Statementioning

confidence: 99%

Surface emission from neutron stars and implications for the physics of their interiors

Özel

2012

Rep. Prog. Phys.

124

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Abstract. Neutron stars are associated with diverse physical phenomena that take place in conditions characterized by ultrahigh densities as well as intense gravitational, magnetic, and radiation fields. Understanding the properties and interactions of matter in these regimes remains one of the challenges in compact object astrophysics. Photons emitted from the surfaces of neutron stars provide direct probes of their structure, composition, and magnetic fields. In this review, I discuss in detail the physics that governs the properties of emission from the surfaces of neutron stars and their various observational manifestations. I present the constraints on neutron star radii, core and crust composition, and magnetic field strength and topology obtained from studies of their broadband spectra, evolution of thermal luminosity, and the profiles of pulsations that originate on their surfaces.

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“…Both of them fit the parameters of the interaction in order to reproduce the empirical saturation properties of nuclear matter extracted from the nuclear-mass table. The latter ones include nonrelativistic Brueckner-Hartree-Fock (BHF) theory (Baldo 1999) and its relativistic counterpart, the Dirac-Brueckner theory (Machleidt 1989;Li et al 1992), the nonrelativistic variational approach also corrected by relativistic effects (Akmal et al 1997(Akmal et al , 1998Morales et al 2002), and more recently the chiral perturbation theory (Kaiser et al 2002). In these approaches the parameters of the interaction are fixed by the experimental nucleonnucleon and/or nucleon-meson scattering data.…”

Section: Brueckner Theorymentioning

confidence: 99%

Protoneutron stars within the Brueckner-Bethe-Goldstone theory

Nicotra¹,

Baldo²,

Burgio³

et al. 2006

A&A

107

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We study the structure of newly born neutron stars (protoneutron stars) within the finite temperature Brueckner-Bethe-Goldstone theoretical approach also including hyperons. We find that for purely nucleonic stars both finite temperature and neutrino trapping reduce the value of the maximum mass. For hyperonic stars the effect is reversed, because neutrino trapping shifts the appearance of hyperons to larger baryon density and considerably stiffens the equation of state.

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Improved variational calculations of nucleon matter

Cited by 59 publications

References 25 publications

Quenching of weak interactions in nucleon matter

Quenching of weak interactions in nucleon matter

Surface emission from neutron stars and implications for the physics of their interiors

Protoneutron stars within the Brueckner-Bethe-Goldstone theory

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