1. A status review on symmetry energy and nuclear structure
蒋维洲
南京东南大学物理系
Collaborators：Bao-An Li，Lie-Wen Chen，Y. L. Zhao, et. al.
Dec.16-19, 2010
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2. Excitations: Giant Resonances, Pigmy resonances, Superdeformation
Introduction
Ground-state properties: s.p. energies, neutron skin, shape coexistence
Excitations: Giant Resonances, Pigmy resonances, Superdeformation
Tensor force: np interactions & exchange terms & symmetry energy
Neutron star crust: transition density & non-Newtonian gravity & pastas & symmetry energy
Neutron star core: hyperons, quarks, meson condensates & Modeling
New forms of symmetry energy: higher order, I(I+1)
Summary
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3. I. (No) Introduction L.W.Chen,et.al., PRC72, 064309 (05)
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5. II. Ground state properties
Approaches: RMF, SHF, Macroscopic+Microscopic model +Shell correction, Shell model,… +BCS/Bogoliubov,
Lattice effective field theory calculations for A = 3,4,6,12 nuclei, PRL104:
Neutron skin thickness in 208Pb
Chen, et.al.
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6. Away from linearity in superheavy and light nuclei
Z=120, N=172,184,198
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8. Model Lagrangian: Further the best fit: FSUGold, PRL95, 122501 (2005);
with
Further the best fit: FSUGold, PRL95, (2005);
Other works: DDME1, Niksic, Vretenar, et.al., PRC 66, (2002);
DDME2: Lalazissis, et.al. PRC71, (2005);
Rho tensor coupling included: Jiang, Zhao, PLB617,33 (2005).
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9. S.p. energies 1p RMF (Z=120, N=172) PRC 81, 044306 (2010).
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10. Level inversion & Symmetry energy
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11. Shape coexistence: A=190 Pb spherical / Hg oblate
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12. III. Excitations: Giant Resonances, Pigmy resonances, Superdeformation
SHF+RPA
RMF+BCS+RPA
RMF+RPA+Resonances +BCS
RMF+RPA+Resonances +Bogoliubov
TDRMF
TDSHF
Vlasov
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13. Giant: Vretenar, et.al. PRC 68, 024310 (2003).
Pigmy: Paar, et.al., PRL94,182501(2005).
Giant: Piekarewicz, PRC69, (R) (2006).
Pigmy: Liang, PRC 75, (2007).
Pigmy: Piekarewicz, arXiv: : 68Ni
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14. De-excitation from superdeformation
Jiang, et.al. EPJA 44, 465 (2010); Commun.Theor.Phys.54,715 (2010).
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15. IV. Tensor force: np interactions & exchange terms&symmetry energy
Dirac equation
np interaction
Tensor force
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20. Revisit the tensor force
Mainly from exchange terms.
Pion & rho: the most important ingredients of the chiral perturbative theory.
Rho meson becomes important in the tensor force due to the in-medium mass dropping associated with the partial restoration of the chiral symmetry.
Vacuum effect on the symmetry energy: vacuum condensate
Applications in superheavy nuclei, nuclei near drip lines, high-spin states…
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21. V. Neutron star crust: transition density & non-Newtonian gravity & pastas & symmetry energy
Negele & Vautherin, NPA 207, 298 (73)
Shen,et.al.,NPA637, 435 (98).
Than, Khan, Giai,. arXiv:  [nucl-th]
Horowitz,et.al, PRC69:045804,2004
Newton, et.al.PRC79:055801,2009
Watanabe, et.al,PRL94:031101,2005
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22. Transition density
Horowitz, Piekarenwicz, PRL86,5647(01): RRPA, namely small amplitude perturbation using the Dyson’s equation
Xu, et.al., PRC79:035802,(09); APJ697:1549,(09) ; PRC81, (10): Dynamical and the thermodynamical methods.
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23. More concern: Non-Newtonian Gravity on transition density
Strong Gravity at surface
Wen,Li,Chen: PRL 103, (2009)
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24. Neutron star core: hyperons, quarks, meson condensates?
Kaon condensate:
Miransky & Shovkovy, PRL88:111601,2002.
Glendenning & Bielich, PRC60:025803,1999.
Zhang, Luo, Li, PRD68:054015,2003.
W. Zuo, A. Li, Z.H. Li, U. Lombardo, PRC70:055802,2004.
A. Odrzywolek, M. Kutschera, Acta Phys.Polon.B40:195,2009.
Li, Zhou, Burgio, & Schulze, PRC81, (2010)
Guo-hua Wang, Wei-jie Fu, et.al., PRC78: (2008)
Guo-yun Shao, Yu-Xin Liu, PLB682:171(2009).
Phenomenological / Chiral model? Self-consistency
Effect of Symmetry energy
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25. Hyperons Glendening, Phys.Rept. 342, 393 (2001);
Schaffner-Bielich, et.al., PRL89, (2002).
Jiang, PLB642, 28 (2006).
Xu, Chen, Ko, Li, PRC81,
(2010).
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26. Symmetry energy and Lambda hyperons
fY=ρY /ρB
Jiang, Nucl-th/ , PLB 642, 28(06)
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27. Density dependence from chirality
Constraining with the chiral symmetry in RMF models
Properties of nucleons and mesons in medium should be constrained by the chiral symmetry and its breaking.
Symmetry energy is dominated by the isovector mesons.
A good candidate is the Walecka model with Brown-Rho scaling: Simple but with chiral limit
Brown,Rho, PRL66, 2720(91)
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28. P.Danielewicz, R.Lacey,W.G.Lynch, Science 298(2002)1592
Pressure of well constructed models
Collective flow data from high energy heavy-ion reactions
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29. Hyperons in nuclear medium with BR scaling
Questions:
(1)How do the Y-N and Y-Y interactions depend on the density?
(2) How to justify the assumption that the density-dependence of YN interaction is similar to NN interaction?
Nonlinearity, interior degrees of freedom
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31. Universal case
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32. SU2 case
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33. Dec.16-19, 2010
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34. Quarks in dense matter and hybrid stars
R.X. Xu, ApJ,596 L59 (2003).
M. Alford,et.al., Astrophys. J.629, 969 (2005).
W.-j.Fu, Wei, Liu, PRL101:181102(2008).
G.X.Peng, A. Li, Lombardo, PRC 77, (2008)
F. Yang, H. Shen, PRC77: (2008).
Xu, Chen, Ko, Li, PRC81, (2010).
A.Li, R.X.Xu, J.F.Lu, MNRAS 402, 2715 (2010).
H. Li, X.L.Luo, H.S. Zong, Phys.Rev.D82,065017(2010).
SD equation, ChPT, NLJ, CS, BR scaling, QMC, Quark cluster & mass scaling, Hadron-Bag model, Bag+pQCD correction…
Meson condensate, chiral condensate, di-quark condensate, CFL, QSC…Beyond standard model?
Symmetry energy vanishes in new phases?
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35. VII. New forms of symmetry energy: higher order, I(I+1)
High orders beyond parabolic approximation
Isospin Physics in Heavy-Ion Collisions at Intermediate Energies, Eds. Bao-An Li and W. Udo Schroder (Nova Science Publishers, Inc, New York, 2001).
Myers & Swiatechi, Ann. Phys. 55, 395(1969); ibid.84, 186 (1974).
Danielewicz, NPA727, 233 (2003).
Xu, et.al., PRC79:035802,(09); APJ697:1549,(09) ; PRC81, (10): Importance of high orders on the transition density of the crust
Chen, et.al. High-order effects on the incompressibility of isospin asymmetric nuclear matter, PRC80: , 2009.
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36. Why not I(I+1)?
RMF study on finite nuclei suggests E ~T(T+1), Ban, et.al. Phys.Lett.B633: ,2006.
In nuclear matter, the parabolic approximation suggests E~T*T
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37. No quantum effect
Radiation correction requires the quantization of Coulomb field
In strong fields, the renormalization required
Calculations of the RRPA with the ring energy is still in progress.
From vacuum polarization of mesons (Chin, AP108, 301 (1977).)
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38. Discussion:
With phase transition to quarks and hyperons, what happens to the symmetry energy?
Tensor force should be constrained by chiral symmetry, or ChPT?
Quantum effects & symmetry energy?
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39. No Summary:
Ground-state properties: s.p. energies, neutron skin, shape coexistence
Excitations: Giant Resonances, Pigmy resonances, Superdeformation
Tensor force: np interactions & exchange terms & symmetry energy
Neutron star crust: transition density & non-Newtonian gravity & pastas & symmetry energy
Neutron star core: hyperons, quarks, meson condensates & Modeling
New forms of symmetry energy: higher order, I(I+1)
Dec.16-19, 2010
西安交大

40. Thanks!
Welcome to Nanjing
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