Ferromagnetic and antiferromagnetic spin-ordering stabilities of asymmetric nuclear matter: Lowest-order constrained variational method

Bigdeli, M.

doi:10.1103/physrevc.82.054312

Cited by 21 publications

(19 citation statements)

References 51 publications

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“…In fact, many effective nuclear interactions of Skyrme [22,23] or Gogny [24] type predict this transition at densities accesible in neutron stars. However, in accordance with the reduction of the spin susceptibility comented above, microscopic calculations based on realistic interactions do not predict such transition at least in the wide range of densities which have been explored [1][2][3][4][5][6][7]. The study of spin-polarization has also been recently considered for nuclear matter and finite nuclei using finite range effective interactions [25].…”

Section: Introductionmentioning

confidence: 95%

Role of correlations in spin-polarized neutron matter

2016

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Background: The possible existence of a phase transition to a ferromagnetic state in neutron matter as origin of the extremely high magnetic fields of neutron stars is still an open issue. Whereas many phenomenological interactions predict this transition at densities accesible in neutron stars, microscopic calculations based on realistic interactions show no indication of it. The existence or non-existence of this transition is a consequence of the different role of nucleon-nucleon correlations in polarized and unpolarized neutron matter. Therefore, to give a definite answer to this issue it is necessary to analyze the behavior of these correlations.Purpose: Using the Hellmann-Feynman theorem we analyze the contribution of the different terms of the nucleon-nucleon interaction to the spin symmetry energy of neutron matter with the purpose of identifying the nature and role of correlations in polarized and unpolarized neutron matter. Methods:The analysis is performed within the microscopic Brueckner-Hartree-Fock approach using the Argonne V18 realistic potential plus the Urbana IX three-body force.Results: Our results show no indication of a ferromagnetic transition as the spin symmetry energy of neutron matter is always an increasing function of density. They show also that the main contribution to it comes from the S=0 channel, acting only in non-polarized neutron matter, in particular from the 1 S0 and the 1 D2 partial waves. Three-body forces are found to play a secondary role in the determination of the spin symmetry energy.Conclusions: By evaluating the kinetic energy difference between the correlated system and the underlying Fermi sea to estimate the importance of correlations in spin-polarized neutron matter, we conclude that non-polarized neutron matter is more correlated than totally polarized one.

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Section: Introductionmentioning

confidence: 95%

Role of correlations in spin-polarized neutron matter

2016

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“…It should be mentioned that the cases δ p = δ n = 0, δ p = δ n and δ p = −δ n are called the unpolarized, ferromagnetic and antiferromagnetic states, respectively [23,24]. Ferromagnetic and antiferromagnetic states may also called polarized states.…”

Section: Resultsmentioning

confidence: 99%

“…By solving these differential equations, we can obtain correlation functions to compute the two-body energy term. For more details see Refs [21,23].…”

Section: Finite Temperature Calculations For Spin Polarized Nu-clmentioning

confidence: 99%

“…In this reference, it has also been shown that for AV 18 potential, the critical temperature is lower than for the CDBONN potential [12]. Employing the self-consistent Hartree-Fock approach using different mean-field interactions of the Skyrme and the Gogny types, it has been indicated that the critical temperatures span a wide range of values, from T c ≃ 14 to 23 MeV showing the effective interaction dependence of the critical properties [13]. In addition, the predicted value of critical temperature for the density-dependent relativistic mean-field models is about 15.7 MeV [14].…”

Section: Introductionmentioning

confidence: 99%

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Influence of spin polarizability on liquid gas phase transition in the nuclear matter

Rezaei

Bigdeli

Bordbar

2015

Int. J. Mod. Phys. E

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In this paper, we investigate the liquid gas phase transition for the spin polarized nuclear matter.Applying the lowest order constrained variational (LOCV) method, and using two microscopic potentials, AV 18 and U V 14 +TNI, we calculate the free energy, equation of state, order parameter, entropy, heat capacity and compressibility to derive the critical properties of spin polarized nuclear matter. Our results indicate that for the spin polarized nuclear matter, the second order phase transition takes place at lower temperatures with respect to the unpolarized one. It is also shown that the critical temperature of our spin polarized nuclear matter with a specific value of spin polarization parameter is in good agreement with the experimental result.1

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“…It was shown that the behavior of spin polarization of neutron matter in the high density region in a strong magnetic field crucially depends on whether neutron matter develops a spontaneous spin polarization (in the absence of a magnetic field) at several times nuclear matter saturation density, or the appearance of a spontaneous polarization is not allowed at the relevant densities (or delayed to much higher densities). The first case is usual for the Skyrme forces [13][14][15][16][17][18][19][20][21][22][23], while the second one is characteristic for the realistic nucleon-nucleon (NN) interaction [24][25][26][27][28][29][30][31][32]. In the former case, a ferromagnetic transition to a totally spin polarized state occurs while in the latter case a ferromagnetic transition is excluded at all relevant densities and the spin polarization remains quite low even in the high density region.…”

Section: Introductionmentioning

confidence: 99%

Finite temperature effects on anisotropic pressure and equation of state of dense neutron matter in an ultrastrong magnetic field

Isayev

Yang

2011

Phys. Rev. C

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Spin polarized states in dense neutron matter with recently developed Skyrme effective interaction (BSk20 parametrization) are considered in the magnetic fields H up to 10 20 G at finite temperature. In a strong magnetic field, the total pressure in neutron matter is anisotropic, and the difference between the pressures parallel and perpendicular to the field direction becomes significant at H > H th ∼ 10 18 G. The longitudinal pressure decreases with the magnetic field and vanishes in the critical field 10 18 < Hc 10 19 G, resulting in the longitudinal instability of neutron matter. With increasing the temperature, the threshold H th and critical Hc magnetic fields also increase. The appearance of the longitudinal instability prevents the formation of a fully spin polarized state in neutron matter and only the states with moderate spin polarization are accessible. The anisotropic equation of state is determined at densities and temperatures relevant for the interiors of magnetars. The entropy of strongly magnetized neutron matter turns out to be larger than the entropy of the nonpolarized matter. This is caused by some specific details in the dependence of the entropy on the effective masses of neutrons with spin up and spin down in a polarized state.

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Ferromagnetic and antiferromagnetic spin-ordering stabilities of asymmetric nuclear matter: Lowest-order constrained variational method

Cited by 21 publications

References 51 publications

Role of correlations in spin-polarized neutron matter

Role of correlations in spin-polarized neutron matter

Influence of spin polarizability on liquid gas phase transition in the nuclear matter

Finite temperature effects on anisotropic pressure and equation of state of dense neutron matter in an ultrastrong magnetic field

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