Relativistic Nuclear Physics: Theories of Structure and Scattering

Celenza, L. S.; Shakin, C. M.

doi:10.1142/0207

Cited by 88 publications

(92 citation statements)

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“…This corresponds to the lowest order exchange by vector and scalar mesons between the probe nucleon and those of the matter. This picture is in agreement with that provided by relativistic nuclear physics [19]. However the four quark condensates (d = 6) also appear to be numerically important.…”

Section: Finite Density Qcd Sum Rulessupporting

confidence: 89%

Three nucleon forces in nuclear matter in QCD sum rules

2017

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We calculate the single-particle nucleon characteristics in symmetric nuclear matter with inclusion of the 3N interactions. The contributions of the 3N forces to nucleon self energies are expressed in terms of the nonlocal scalar condensate (d = 3) and of the configuration of the four-quark condensates (d = 6) in which two daiquiri operators act on two different nucleons of the matter. The most important part of the contribution of the four-quark condensate is calculated in a model-independent way. We employed a relativistic quark model of nucleon for calculation of the rest part. The density dependence of the vector and scalar nucleon self energies and of the single-particle potential energy are obtained. Estimations on contributions of the 4N forces to the nucleon self energies are made.

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Section: Finite Density Qcd Sum Rulessupporting

confidence: 89%

Three nucleon forces in nuclear matter in QCD sum rules

2017

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“…Only in this window [31,32] one obtains positive values for c N (or b N ≫ |c N |) and more moderate meson fields, so that the problem of negative nucleon Dirac masses is avoided. The reasons given for this choice rest on a reproduction of the effective mass (∼ 0.83 m N ) [8,36], however a closer inspection according to a more elaborate investigation by Celenza and Shakin shows that values of again 0.6 m N are more appropriate for the Dirac mass [37] (see also Ref. [38]).…”

Section: B) Comparison Of the Different Approximationsmentioning

confidence: 99%

“…22). For the EOSs considered here the only possible enhanced cooling processes are the nucleon [36,37] n → p + l − +ν l (III.42) and the hyperon direct Urca processes [57]as well as their inverse reactions. Here, l denotes electrons and muons.…”

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confidence: 99%

Neutron Star Properties with Relativistic Equations of State

Huber

Weber

Weigel

et al. 1998

Int. J. Mod. Phys. E

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We study the properties of neutron stars adopting relativistic equations of state of neutron star matter, calculated in the framework of the relativistic Brueckner-Hartree-Fock approximation for electrically charge neutral neutron star matter in beta-equilibrium. For higher densities more baryons (hyperons etc.) are included by means of the relativistic Hartree-or Hartree-Fock approximation. The special features of the different approximations and compositions are discussed in detail. Besides standard neutron star properties special emphasis is put on the limiting periods of neutron stars, for which the Kepler criterion and gravitation-reaction instabilities are considered. Furthermore the cooling behaviour of neutron stars is investigated, too. For comparison we give also the outcome for some nonrelativistic equations of state. I IntroductionA necessary ingredient for solving the structure equations for (rotating) neutron stars (NS) is the equation of state (EOS) [1]. For NSs the EOS has to cover a wide range of densities ranging from super-nuclear densities (up to 5 to 10 times normal nuclear matter density) in the star's core down to the density of iron at the star's surface. At present, neither heavy-ion reactions nor NS data are capable to determine the EOS accurately, and the behaviour of high-density matter is still an open and one of the most challenging problems in modern physics, containing many ingredients from different branches of physics. The theoretical determination of the EOS over such an enormous range has therefore to rely mainly on theoretical arguments and extrapolations for which no direct experimental confirmation exists. The best one can do in such a situation is a step-by-step improvement of the available models for the EOS. Since the central density of a NS is so extreme, both the Fermi momenta and the effective nucleon mass are of the order of 500 MeV, one should prefer a relativistic description [2]- [9].Neutron star matter differs from the high density systems produced in heavy ion collisions by two essential features: a) Matter in high energy collisions is still governed by the charge symmetric nuclear force while neutron star matter (NSM) is bound by gravity. Since the repulsive Coulomb force is much stronger than the gravitational attraction, NSM is much more asymmetric than "standard" matter. b) The second essential difference is caused by the weak interaction time scale of ∼ 10 −10 s, which is small in comparison with the lifetime of the star, but large in comparison with the characteristic time scale of heavy ion reactions. For that reasons "normal" matter is subject to the constraints of isospin symmetry and strangeness conservation, but NSM has to obey the constraints of charge neutrality and generalized beta-equilibrium with no strangeness conservation. It is obvious from these considerations that NSM is an even more theoretical object than nuclear "normal" matter, with a rather complex structure [2]- [9].Due to these features one can adopt the following structure o...

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“…In recent years considerable efforts have been devoted to the development of relativistic nuclear models, whose basis is usually a relativistic Lagrangian containing nucleons and mesons [1][2][3]. On the other hand, the traditional concept of interparticle potential has proved to be quite useful in nuclear physics and rather sophisticated techniques of calculation have been developed within the hamiltonian formalism.…”

Section: Introductionmentioning

confidence: 99%

Relativistic Hamiltonians in many-body theories

1996

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We discuss the description of a many-body nuclear system using Hamiltonians that contain the nucleon relativistic kinetic energy and potentials with relativistic corrections. Through the Foldy-Wouthuysen transformation, the field theoretical problem of interacting nucleons and mesons is mapped to an equivalent one in terms of relativistic potentials, which are then expanded at some order in 1/m N . The formalism is applied to the Hartree problem in nuclear matter, showing how the results of the relativistic mean field theory can be recovered over a wide range of densities.

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Relativistic Nuclear Physics: Theories of Structure and Scattering

Cited by 88 publications

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Three nucleon forces in nuclear matter in QCD sum rules

Three nucleon forces in nuclear matter in QCD sum rules

Neutron Star Properties with Relativistic Equations of State

Relativistic Hamiltonians in many-body theories

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