EOS of neutron-rich matter and pure neutron matter

2012 ◽  
Vol 55 (3) ◽  
pp. 443-449 ◽  
Author(s):  
Kaan Manisa
Keyword(s):  
Neutron Matter ◽  
Pure Neutron Matter

scholarly journals Effects of Magnetization on Structure Parameters of Neutron Stars

1987 ◽  
Vol 125 ◽  
pp. 451-451
Author(s):  
Q.M. Wang ◽  
S.H. Gao
Keyword(s):  
Magnetic Susceptibility ◽  
Neutron Stars ◽  
Ferromagnetic State ◽  
Neutron Matter ◽  
Variation Method ◽  
Repulsive Core ◽  
Structure Parameters ◽  
Ferromagnetic Transition ◽  
Order Constraint ◽  
Pure Neutron Matter

We took the magnetic susceptibility χ as a criterion in this study and supposed that the system of neutron matter has a ferromagnetic transition as 1/χ 0. The magnetic susceptibility of pure neutron matter at zero temperature was calculated by means of Owen's lowest order constraint variation method. The following results were obtained: if the interaction between neutron and neutron was the Reid soft-core potential, then no transition to ferromagnetic state was found to occur; if the interaction was HJ, IY potentials, the neutron matter would undergo a transition. These results indicate that the existence of ferromagnetic state depends on the form of potentials. If the interaction between particles is attractive, it will not profit the existence of ferromagnetic state, while the interaction between neutrons has a repulsive core, it will profit the existence of ferromagnetic state. We also calculated the equation of state and structure parameters of neutron stars. It showed that the energy of ferromagnetic state is lower than that of nonferromagnetic one and the ferromagnetic state is more stable. In other words, the ferromagnetic state may exist in neutron stars. We can readily find that ferromagnetic state has some influence on structure parameters of neutron stars, the magnitude of this effect depends on the form of potentials and the values of these structure parameters with ferromagnetism are within the allowed range. In this paper, the possibility existing the ferromagnetic state has been dsicussed. By a rough estimate, the magnetic field strength coming from the complete ferromagnetic state is about 1015 Gauss at ρ ∼ 1015 g/cm3. We assume that this is a possible origin of the strong magnetic fields in neutron stars. If there exists a ferromagnetic state in neutron stars, it will have a substantial influence on the gravitaional collapse theory, neutron superfluid and proton superconductivity.

scholarly journals Bulk Properties of Symmetric Nuclear and Pure Neutron Matter

2013 ◽  
Vol 04 (05) ◽  
pp. 37-41 ◽  
Author(s):  
Khaled Hassaneen ◽  
Hesham Mansour
Keyword(s):  
Neutron Matter ◽  
Bulk Properties ◽  
Pure Neutron Matter

scholarly journals Benchmark calculations of pure neutron matter with realistic nucleon-nucleon interactions

2020 ◽  
Vol 101 (4) ◽  
Author(s):  
M. Piarulli ◽  
I. Bombaci ◽  
D. Logoteta ◽  
A. Lovato ◽  
R. B. Wiringa
Keyword(s):  
Nucleon Nucleon ◽  
Neutron Matter ◽  
Pure Neutron Matter ◽  
Nucleon Interactions

Triplet superfluidity in neutron matter with Skyrme forces at subnuclear and supranuclear densities in a strong magnetic field

Open Physics ◽  
2011 ◽  
Vol 9 (4) ◽  
Author(s):  
Alexander Tarasov
Keyword(s):  
Magnetic Field ◽  
Phase Transitions ◽  
Strong Magnetic Field ◽  
Critical Density ◽  
Outer Core ◽  
Neutron Matter ◽  
P Wave ◽  
Phase Transition Temperatures ◽  
Pure Neutron Matter ◽  
Analytical Formulae

AbstractWithin a generalized non-relativistic Fermi-liquid approach we have found general analytical formulae for phase-transition temperatures T c,1(n, H) and T c,2(n, H) (which are nonlinear functions of density, n, and linear of magnetic field, H) for phase transitions in spatially uniform, dense, pure neutron matter from normal to superfluid states with spin-triplet p-wave pairing (similar to anisotropic superfluid phases 3He - A1 and 3He - A2) in steady and homogeneous sufficiently strong magnetic field (but |µn|H ≪ E c < ɛ F(n), where µn is the magnetic dipole moment of a neutron, E c is the cutoff energy and ɛ F(n)is the Fermi energy in neutron matter). General formulae for T c,1,2(n,H) are valid for arbitrary parameterization of the effective Skyrme forces in neutron matter. We have used for definiteness the so-called SLy2, Gs and RATP parameterizations of the Skyrme forces with different exponents in their power dependence on density n (at sub- and supranuclear densities) from the interval 0.7 n 0 ≲ n < n c(Skyrme)< 2 n 0, where n 0 =0.17 fm−3 is the nuclear density and n c(Skyrme)is the the critical density of the ferromagnetic instability in superfluid neutron matter. These phase transitions might exist in the liquid outer core of magnetized neutron stars.

Calculation of Landau's fermi-liquid parameters in pure neutron matter

1973 ◽  
Vol 43 (4) ◽  
pp. 263-266 ◽  
Author(s):  
S.-O. Bäckman ◽  
C.-G. Källman ◽  
O. Sjöberg
Keyword(s):  
Fermi Liquid ◽  
Neutron Matter ◽  
Pure Neutron Matter

Abnormal state of pure neutron matter: Effects of correlations

1975 ◽  
Vol 57 (2) ◽  
pp. 183-185 ◽  
Author(s):  
C.-G. Källman ◽  
S.A. Moszkowski
Keyword(s):  
Neutron Matter ◽  
Matter Effects ◽  
Abnormal State ◽  
Pure Neutron Matter
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