Magnetic properties of neutron matter

Pfarr, Joachim

doi:10.1007/bf01380457

Cited by 10 publications

(5 citation statements)

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“…To remedy such a behaviour and to get agreement with the results obt.ained by realistic forces which are in turn related to the phase shifts, we allowed the parameters to change from the first set. The second set of parameters shows good agreement with Haensel for RHC potential [8], Moszkowski (curve C) [ 141, Pandharipande et d. [16] and the results of Pfarr [17] (curve I)) (see Fig. 3).…”

Section: Resiilts and Discussionsupporting

confidence: 60%

Neutron Matter Properties Using Skyrme Interaction

et al. 1989

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A b s t r a c t The purpose of the present work is t o extend earlier nuclear matter calculations to study the properties of neutron matter. The binding energy per particle, symmetry energy, single particle potential, effective mass, and magnetic susceptibility are calculated using a modified skyrme interaction. These are calculated as a function of the Fermi momentum kr in the range 0 < kr < 2 fm-l. Two sets of the interaction parameters are obtained by fitting the interaction parameters using the available informahion on neutron matter. Relativistic corrections to the order 1/c2 are also calculated. The relativistic corrections are very small and they increase as kf is increased.

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Section: Resiilts and Discussionsupporting

confidence: 60%

Neutron Matter Properties Using Skyrme Interaction

et al. 1989

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“…In previous calculations in the non-relativistic formalism using realistic interactions, one usually does not find such a ferromagnetic transition [18,19] or if there is such a possibility, it occurs at densities [19] not realisable in the context of neutron stars. In a relativistic framework, one finds that the simple σ + ω model [20] does not suggest any such transition.…”

Section: Ferromagnetic Phase Transitionmentioning

confidence: 95%

“…In the framework of Hartree-Fock theory, employing hard and also soft core potentials, Pfarr [18] does not get such a ferromagnetic transition. A similar conclusion is reached by Forseth and Ostgaard [19] who made the calculations in the lowest order constrained variational method of Pandharipande using soft core potentials; with a hard core potential a transition to the ferromagnetic state was seen to occur though at ∼ 30 ρ o , where ρ o is the normal nuclear matter density.…”

Section: Introductionmentioning

confidence: 98%

Spin polarised nuclear matter and its application to neutron stars

Maheswari

Basu

et al. 1997

Nuclear Physics A

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An equation of state(EOS) of nuclear matter with explicit inclusion of a spin-isospin dependent force is constructed from a finite range, momentum and density dependent effective interaction. This EOS is found to be in good agreement with those obtained from more sophisticated models for unpolarised nuclear matter. Introducing spin degrees of freedom, it is found that at density about 2.5 times the density of normal nuclear matter the neutron matter undergoes a ferromagnetic transition. The maximum mass and the radius of the neutron star agree favourably with the observations. Since finding quark matter rather than spin polarised nuclear matter at the core of neutron stars is more probable, the proposed EOS is also applied to the study of hybrid stars. It is found using the bag model picture that one can in principle describe both the mass and size as well as the surface magnetic field of hybrid stars satisfactorily.Comment: 26 pages, 11 figures available on reques

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“…This model is also realized in helium-3 (9), but it turns into solid and not into a ferromagnetic phase at high pressure. It has also been applied to neutrons in neutron stars (10).…”

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confidence: 99%