Relativistic description of Exotic Nuclei and Magnetic rotation

1. Relativistic description of Exotic Nuclei and Magnetic rotation 孟 杰Jie Meng • 北京大学物理学院School of Physics/Peking U • 兰州重离子加速器国家实验室核理论中心 HIRFL/Lanzhou • 中国科学院理论物理研究所 Institute for Theor.Phys./AS

2. Contents • New Effective Interactions in RMF • Nuclear matter and neutron star • Finite Nuclei and halos • SRHWS: replacement of HO basis • New Magic number in Super-heavy nuclei • Magnetic rotation and Chiral bands

3. Effective interaction for RMF Start: simple  models Incompressibility requires the self-coupling of : NL1 and NLSH etc. Follow the Dirac-Brueckner Theory / Instability at high density a) the self-coupling of  : TM1 b) correct incompressibility: NL3 c) DD effective interactions (TW99,DD-ME1,) The problem for the correction of CM a) Phenomenological ( -3/4 41 A -1/3 , -17.2 A -0.2 ) b) Microscopically ( - 1/2MA < PCM 2 > ) So far, only in TM2 and DDME1, the correction of CM are better treated. Effective interaction with the microscopically correction of CM are needed. Extrapolation for low and high nuclear matter

4. Microscopic & Phenomenological ECM

5. Nonlinear & DD RMF Lagrangian density: Nonlinear RMF DD RMF Five constraints

6. Equations of Motion for DD RMF : Rearrangement terms:

7. Parameter sets PK1, PK1r and PKdd

8. DD for PKDD, TW99 and DD-ME1

9. E for PKDD, PK1 and PK1r

10. rch for PKDD, PK1 and PK1r

11. Nuclear matter The density dependencies of various effective interaction strengths in relativistic mean field are studied and carefully compared for nuclear matter. The corresponding influences of those different density dependencies are presented and discussed on mean field potentials, saturation properties of nuclear matter.

12. Properties for nuclear matter TM2, TM1, NL2,NLSH

13. Nuclear matter

14. Density dependence of Interaction strengths in Nuclear Matter

15. Potentials in nuclear matter

16. Neutron Star The density dependencies of various effective interaction strengths in relativistic mean field are studied and carefully compared for neutron star. The corresponding influences of those different density dependencies are presented and discussed on mean field potentials, equations of state, maximum mass and corresponding radius in neutron star.

17. Density dependence of Interaction strengths in Neutron Star

18. Potentials in Neutron Star

19. Binding energy per baryon in Neutron Star

20. Particle n, p, e- and - densities in Neutron Star

21. EOS for Neutron Star

22. Neutron Star Center density vs. masses Radius vs. masses

23. Finite Nuclei in DD RMF New parameter sets for Lagrangian density, PK1, PK1r, PKDD are able to provide an excellent description not only for the properties of nuclear matter but also for the nuclei in and far from the valley of beta-stability with the center-of-mass correction included in a microscopic way.

24. Pb isotopes in RCHB

25. Isotope shift in Pb isotopes

26. Single particle energy in RCHB

27. Sn isotopes in RCHB

28. Single particle energy in RCHB

29. Ni isotopes in RCHB

30. Single particle energy in RCHB

31. Single particle energy in RCHB

32. Halos and Giant halos Recent work on the existence of giant halo and hyperon halo in relativistic continuum Hartree-Bogoliubov (RCHB) theory is reviewed. Experimental support of giant halos in Na and Ca isotopes near the neutron drip line is discussed and the progress on deformed halo is presented.

33. 巨晕 J.Meng and P. Ring, 《Physical Review Letters》80 (1998)460

34. The Exp. and calculated S2n by RCHB for Ca, Ni, Zr, Sn and Pb isotopes J.Meng, et al.，《Physical Review》C 65 (2002 ) 41302(R) Giant Halos

35. Two neutron Separation Energy

36. Development of neutron skin

37. Neutron halos in hyper Ca isotopes Lu, et al., Euro. Phys. J . A17，19-24 (2003)

38. Hyper Nuclei 13CΛ13C 2Λ Hyperon halo nuclei：13C3Λ Lu HF, and Meng JChin. Phys. Lett. 19 (12): 1775-1778 DEC 2002.

39. Existence of deformed halo ? • Otsuka et al. have studied the structure of 11Be and 8B with a deformed Woods-Saxon potential considered quadrupole deformation as a free parameter adjusted to the data. T.Otsuka,A.Muta,M.Yokoyama,N.Fukunishi,and T.Suzuki,Nucl.Phys.A588, 113c(1995). • Based on a spherical one-body potential: the positions of experimental drip lines are consistent with the spherical picture;I.Tanihata,D.Hirata,and H.Toki, Nucl.Phys.A583,769 (1995). • Using the deformed single-particle model，the existence of the deformed halo is doubted ?T. Misu, W. Nazarewicz, S. Aberg, Nucl.Phys. A614 (1997) 44-70. nucl-th/9612016 : Deformed nuclear halos

40. Progress and Challenge • Deformation and Continuum: (DRCHB) • Coupled channel equations in coordinate space • The formalism and code for DRCHB • For given pairing potential DRCHB works well • Full self-consistence is under construction…

41. Limits of present methods RMF in Woods-Saxon basis • RMF in H.O. basis: unsuitable for exotic nuclei • In coordinate space: difficult for deformed nuclei

42. Development of SRHWS RMF Theory - Shan-Gui Zhou, Jie Meng, Peter Ring, Phys.Rev.C Lagrangian where

43. RMF Theory: field equations Dirac equations for nucleons K-G equations for mesons

44. Relativistic Hartree theory for spherical nuclei

45. SRHSWS

46. SRHDWS

47. Convergence with energy cutoff

48. Convergence with Dirac Sea

49. Convergence of SRHWS theory

50. Convergence of density distribution