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Symmetry energy with non-nucleonic degrees of freedom

Symmetry energy with non-nucleonic degrees of freedom. Wei-Zhou Jiang Department of Physics, Southeast University, China Collaborators: Bao-An Li, et al. Outline. Introduction Hyperons, quarks, dark matter? Symmetry energy and quarks & hyperons Interaction of quarks and its effects

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Symmetry energy with non-nucleonic degrees of freedom

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  1. Symmetry energy with non-nucleonic degrees of freedom Wei-Zhou Jiang Department of Physics, Southeast University, China Collaborators: Bao-An Li, et al. Aug. 19-22, 2013 @ TAMU

  2. Outline • Introduction • Hyperons, quarks, dark matter? • Symmetry energy and quarks & hyperons • Interaction of quarks and its effects • In neutron stars, effect of dark matter? • Summaries Aug. 19-22, 2013 @ TAMU

  3. SYMMETRY ENERGY Liquid-drop model for nuclei — E= W. D. Myers, W.J. Swiatecki, P. Danielewicz,…… In isospin asymmetric matter: Aug. 19-22, 2013 @ TAMU

  4. Where it is the matter, there is the symmetry energy. Aug. 19-22, 2013 @ TAMU

  5. Fuchs, et.al., arXiv:nucl-th/0511070 L.W.Chen,et.al., PRC72, 064309 (05) Aug. 19-22, 2013 @ TAMU

  6. Diverse trends from data 1. Xiao, Li, et.al PRL102, 062502 (2009) 2. Feng&Jin, PLB683 (2010) 140 3. P. Russotto,W. Trauntmann, Q.F. Li et al., PLB697, 471(2011) 31.6(ρ/ρ)γ,with γ=0.9+/-0.4：almost linear Aug. 19-22, 2013 @ TAMU

  7. The dense the matter, the uncertain the symmetry energy Factor to soften greatly the Symmetry Energy: • Tensor force C. Xu and B. A. Li, PRC81, 064612: I. Vidana, A. Polls, and C. Providencia, PRC 84, 062801(R) . Aug. 19-22, 2013 @ TAMU

  8. Significant points: • To go ahead to deal with Tensor force with pion & rho: the most important ingredients of the chiral perturbative theory in Density dependent RHF approach: the simple, self-consistent and covariant framework. • Here, we just go beyond this point to discuss contributions of non-nucleonic components to the symmetry energy. Aug. 19-22, 2013 @ TAMU

  9. Non-nucleonic degrees of freedom • Threshold for hyperons reaches at high densities; 2ρ0-4ρ0 • Hadron-Quark transition may occur for nucleon overlaps >2ρ0 • In astrophysical extraction of the symmetry energy, there may be the effect of unknown dark matter. • What is the effect of these components in dense matter? Matter changes, so does the interaction, so does the symmetry energy? Aug. 19-22, 2013 @ TAMU

  10. Model Lagrangian (RMF) : with Hyperons: Aug. 19-22, 2013 @ TAMU

  11. EoS with inclusion of hyperons Definition of symmetry energy: at given hyperon fraction. for charge neutral and chemical equilibrated matter Aug. 19-22, 2013 @ TAMU

  12. RMF models: SLC and SCLd Demorest, et al., Nature 467, 1081(2010)：PSR J1614-2230 Jiang，Li，and Chen, PLB653，184 （07）； PRC76, 054314 (07); ApJ756，56（12） RMF model NL3: Lalazissis, et. al. PRC 55, 540(97). Aug. 19-22, 2013 @ TAMU

  13. Aug. 19-22, 2013 @ TAMU

  14. Symmetry energy with quarks Step 1: no interaction between Qs & Ns a function of α Y is the quark phase proportion, determined by Gibbs conditions. We just consider the symmetric matterα=0 Aug. 19-22, 2013 @ TAMU

  15. Critical density Calculation detail: Charge chemical potential neglected here! Aug. 19-22, 2013 @ TAMU

  16. Aug. 19-22, 2013 @ TAMU

  17. Symmetry energy of quark flavor Aug. 19-22, 2013 @ TAMU

  18. With Λ hyperons Jiang et al,PRC87, 064314(2013) Aug. 19-22, 2013 @ TAMU

  19. Questions: • Clear model dependence of the transition density and the symmetry energy • Why the transition density is so small as the strange quarks are included? • Chemical potential and mechanical equilibriums should be corrected by interactions between quarks Aug. 19-22, 2013 @ TAMU

  20. Grand thermodynamical potential of quarks Weissenborn, et al, arXiv:1102.2869 Alford, et al, APJ629:969(2005) Step 2: interactions for quarks Mechanical and chemical equilibriums Aug. 19-22, 2013 @ TAMU

  21. Preliminary results: No QCD correction 2-flavor QCD corr., a4=0.6 3-flavor Aug. 19-22, 2013 @ TAMU

  22. No QCD corrections No correction to asymmetric part Aug. 19-22, 2013 @ TAMU

  23. Aug. 19-22, 2013 @ TAMU

  24. Symmetry energy: calculation is yet to make • Step 3: interaction between Q’s & N’s Aug. 19-22, 2013 @ TAMU

  25. Dark matter in neutron stars Only gravitational attraction between normal matter and dark matter Aug. 19-22, 2013 @ TAMU

  26. Symmetry energy extraction with Dark matter Steiner:PRL 108, 081102 (2012) Effect of Dark Matter? Guillot et al. 2013, ApJ 772 Aug. 19-22, 2013 @ TAMU

  27. DM with interactions Aug. 19-22, 2013 @ TAMU

  28. Summary • Non-nucleonic degrees of freedom do affect the symmetry energy. • Experimental extraction of symmetry energy at high densities should be of caution about the effects of new phases • The astrophysical extraction of symmetry energy could undergo the influence of celestial dark matter that belongs to an unknown universe. Aug. 19-22, 2013 @ TAMU

  29. Thank you for your attention! Aug. 19-22, 2013 @ TAMU

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