2012/12/17 by Alexander N. Tarasov, A N Tarasov
Physics and Astronomy · #Cold Atom Physics and Bose-Einstein Condensates #Nuclear physics research studies #Pulsars and Gravitational Waves Research #astro-ph.SR #cond-mat.stat-mech #nucl-th
paper · pdf · doi:10.1088/1742-6596/400/3/032101
published as Journal of Physics: Conference Series, 400 (2012) 032101 · 4 pages, 2 figures; Proceedings of the 26th International Conference on Low Temperature Physics (LT26), Beijing, China, 10-17 August 2011
openalex publication_date 2012/12/17 · arxiv created 2013/01/23 · arxiv updated 2013/01/24 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/30
A generalized non-relativistic Fermi-liquid approach was used to find analytical formulas for temperatures T c1 ( n , H ) and T c2 ( n , H ) (which are functions nonlinear of density n and linear of magnetic field H ) of 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 3 He-A 1 and 3 He-A 2 ) in steady and homogeneous strong magnetic field (but |μ n | H ≪ E c < ∊ F (n) , where μ n is the magnetic dipole moment of a neutron, E c is the cutoff energy and ∊ F (n) is the Fermi energy in neutron matter). General formulas for T c1 , 2 ( n , H ) (valid for arbitrary parameterization of the effective Skyrme interaction in neutron matter) are specified here for generalized BSk18 parameterization of the Skyrme forces (with additional terms dependent on density n ) on the interval 0.3 n 0 < n < n c (BSk18) ≍ 2.7952 · n 0 , where n 0 = 0.17 fm −3 is nuclear density and at critical density n c (BSk18) triplet superfluidity disappears, T c0 ( n , c H = 0) = 0. Expressions for phase transition temperatures T c0 ( n )<0.09MeV (at E c = 10MeV) and T c1 , 2 ( n , H ) are realistic non-monotone functions of density n for BSk18 parameterization of the Skyrme forces (contrary to their monotone increase for all previous BSk parameterizations). Phase transitions to superfluid states of such type might occur in liquid outer core of magnetars (strongly magnetized neutron stars).