Spin-triplet superfluidity of neutron matter with Skyrme forces in strong magnetic field near Tc
A dense homogeneous superfluid pure neutron matter (SPNM) with the effective Skyrme forces (depending on the density n of the neutrons) and with spin-triplet p–wave pairing (similar to ³He-A₁ and ³He-A₂) in a strong uni-form static magnetic field H is studied in the framework of a generalized non-re...
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| Date: | 2007 |
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| Main Author: | |
| Format: | Article |
| Language: | English |
| Published: |
Національний науковий центр «Харківський фізико-технічний інститут» НАН України
2007
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| Series: | Вопросы атомной науки и техники |
| Subjects: | |
| Online Access: | http://dspace.nbuv.gov.ua/handle/123456789/111057 |
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| Journal Title: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Cite this: | Spin-triplet superfluidity of neutron matter with Skyrme forces in strong magnetic field near Tc / A.N. Tarasov // Вопросы атомной науки и техники. — 2007. — № 3. — С. 418-423.— Бібліогр.: 20 назв. — англ. |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine| Summary: | A dense homogeneous superfluid pure neutron matter (SPNM) with the effective Skyrme forces (depending on the density n of the neutrons) and with spin-triplet p–wave pairing (similar to ³He-A₁ and ³He-A₂) in a strong uni-form static magnetic field H is studied in the framework of a generalized non-relativistic Fermi-liquid theory. General formulas (valid for arbitrary parameterization of the Skyrme forces) are derived analytically for the phase transition temperatures Tc1,₂ of the neutron matter from normal to superfluid states of ³He-A1 and ³He-A₂ types, respectively. The functions Tc₁,₂(H,n) are linear with respect to H (up to sufficiently high magnetic fields) and are non-monotone functions of density. Figures for (Tc₁(H,n)−Tc₂(H,n))/H are plotted in the range 0.8n₀≤n≤3n₀ (n₀=0.17 fm⁻³ is the saturation density of the symmetric nuclear matter) for selected RATP, SkO’ and Gs parame-terizations of the Skyrme forces which have different power dependences on density. Such phases of dense SPNM may exist in cores of magnetized neutron stars. |
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