in neutron star matter at finite temperatures Adam Szmagliski, - PowerPoint PPT Presentation

The Structure and Signals of Neutron Stars, from Birth to Death GGI, Florence, 24-28 March 2014 Properties of localized protons in neutron star matter at finite temperatures Adam Szmagliński, Sebastian Kubis, Włodzimierz Wójcik Institute of Physics, Cracow University of Technology

Realistic Nuclear Models: Skyrme (SI’, SII’, SIII’, SL, Ska, SKM, SGII, RATP, T6) 1. Myers- Świątecki (MS) 2. 3. Friedman-Pandharipande-Ravenhall (FPR) 4. UV14+TNI (UV) 5. AV14+UVII (AV) 6. UV14+UVII (UVU) 7. A18 A18+ δ v 8. 9. A18+UIX 10. A18+ δ v+UIX*

Symmetry Energy of Nuclear Matter     1          2 x n P / n E n , x E n , E n 2 x 1 S   2    2   1 E n , x  E n  S 2 8 x 1  x 2

Small values of the symmetry energy: 1. Low proton concentration 2. Charge separation instability • realized eg. through proton localization

Model of Proton Impurities in Neutron Star Matter (M. Kutschera, W. Wójcik) We divide the system into spherical Wigner-Seitz cells, each of them enclosing a single proton: 1  V The volume of the cell: n P     E V n N n , The energy of the cell of uniform phase: 0 P       P      n , n n n n N P N P N         E n V n 0 P N N

3      2   2 3 r 4        2 r R exp   P P   2   3 4 R P         2                2           * 3     E r n r r n r B n r d r L P P P N   2 m   P V 9      E E E L 0 2 8 m R P P      2                     dn r              2   4 r p r n r n n r n B dr P P N N N     dr   0          * p r r r where P P

The self-consistent variational method      n r r We look for such functions and , that minimize functional:                             3 * 3   f n r , r E n r n d r E r r d r 1 P N P P   V V  , E - Lagrange multipliers boundary conditions:                 3 * 3 0 1 0 n r n d r r r d r N P P V V

     * n r r By differentiation with respect to and we obtain P following Euler-Lagrange equations:   1                       2 r n r n r E r P P P N P P P 2 m P             2 n r         d n r dn r            * P r r n r 2 B r r 2 0      P P N N 2   n r dr dr         r N n R - variational parameter N P

n loc Potential R loc P MS 1.033 0.906 SI’ 0.351 1.570 SII’ 0.361 1.688 SIII’ 0.337 1.552 SL 0.964 1.384 Ska 1.016 0.804 SKM 0.979 1.330 FPR 0.721 1.262 UV14+TNI 0.731 1.209 AV14+UVII 0.789 0.971 UV14+UVII 0.766 0.913 A18 1.493 1.136 A18+ δ v 1.627 0.915 A18+UIX 0.645 0.911 A18+ δ v+UIX* 0.819 0.878

Properties of nuclear matter at T>0 We minimize the free energy difference         F E T 1 x S xS N P Kinetic energy density      2 5 / 2    * 2 m T J   N , P N , P 3 / 2 N , P 2 2 Where the entropy per baryon      5 1 1 1 3 / 2     * 2 S m T J  N , P  N , P 3 / 2 N , P N , P 2 3 n 2 2 , N P

 The unknown quantity comes from: N , P      2 3 / 2   * n 2 m J  N , P  N , P 1 / 2 N , P 2 2      x    Fermi integrals are defined J dx    x 1 e 0 Nucleon chemical potentials are the derivatives  of the free energy density f    N , P n N , P

Conclusions 1. Symmetry energy implies the inhomogeneity of dense nuclear matter in neutron stars. 2. Proposal of self-consistent variational method – neutron background profile as a solution of variational equation with parameter (mean square radius of proton wave function). 3. Localization of protons as an universal state of dense nuclear matter in neutron stars. 4. Nonzero temperature lowers the localization threshold density and diminishing the size of the proton wave function. 5. Localization is still present at very high temperature.

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