1 / 17

Nuclear excitations in relativistic nuclear models

Nuclear excitations in relativistic nuclear models. 1 Akihiro Haga , 1 Hiroshi Toki, 1 Setsuo Tamenaga, and 2 Yataro Horikawa 1. RCNP Osaka University 2. Juntendo University. 8/1-8/3 現代の原子核物理 - 多様化し進化する原子核の描像 @KEK. Introduction.

kaida
Télécharger la présentation

Nuclear excitations in relativistic nuclear models

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Nuclear excitations in relativistic nuclear models 1Akihiro Haga, 1Hiroshi Toki, 1Setsuo Tamenaga, and 2Yataro Horikawa 1. RCNP Osaka University 2. Juntendo University 8/1-8/3 現代の原子核物理-多様化し進化する原子核の描像@KEK

  2. Introduction • The relativistic nuclear model has succeed to describe the nuclear ground-state properties, mainly due to the large spin-orbit force arising from the (small) relativistic effective mass. • Recently, however, it is reported that there are discrepancies in the nuclear excitations calculated by the relativistic model, and it presumably originated by the relativistic effective mass. • In the conventional relativistic model, the negative-energy state is not used for the construction of ground state (no-sea approximation). This treatment is crucial to lead to small effective mass. We thought important to reconsider the negative-energy contribution (vacuum polarization)

  3. What is the vacuum polarization? Vacuum of electron-positron field is polarized by electromagnetic field generated by nuclear charge. Vacuum of nucleon-anti-nucleon field is also polarized by nuclear force! e - e+

  4. Vacuum polarization in Walecka model ω σ+ω potential for the positive-energy state -ω σ σ-ω potential for the negative-energy state

  5. Instability of vacuum polarization Nucleons Total No solution Vacuum Scalar potential as a function of coupling constant gσ in nuclear matter. Effective mass, should be large!!

  6. Computation of the Dirac-sea effect –Derivative expansion– One-loop vacuum contribution to Lagrangian: is expanded in terms of the derivatives of meson fields as, Then, the functional coefficients are given as, A. Haga et. al., Phys. Rev. C70, 064322(2004)

  7. Effective Lagrangian of the Walecka modelwith the vacuum contribution Tensor coupling term G. Mao, Phys. Rev. C67, (2003) A. Haga, nucl-th/0601041 Leading-order derivative expansion Parameters, gσ , gω , gρ , mσ… are selected with nuclear matter properties and ground-state properties of finite spherical nuclei (binding energy and charge radius).

  8. Fully-consistent RPA calculation RPA equation : Uncorrelated polarization tensor obtained by RHA Green function Density part Feynman (vacuum polarization) part

  9. Vacuum-polarization (Feynman) part Effective action Mesons at initial and final vertices Vacuum polarization is given by the functional derivatives of the effective action. A B A. Haga et al., Phys. Rev. C72 (2005)

  10. Isoscalar giant quadrupole resonances The model with the vacuum polarization reproduces the data on the ISGQR !

  11. Excitation energies of ISGQR as a function of the relativistic effective mass. The relativistic effective mass m*/m~0.8 is required to reproduce experimental ISGQR energies.

  12. Two-body Interaction; fπ=0.08, mπ=139MeV g’ is obtained by fitting with the peak of the Gamow-Teller resonance in 208Pb. Then, the value of g’ is model-dependent as, g’ is sensitive to the value of which is the strength of tensor force.

  13. GTRDistribution Fitting g’ with the GTR peak, 19.2MeV, the shape becomes very similar. Exp. 60-70% Cut Off energy 50MeV. The rest comes from the excitations larger than 50MeV＋antinucleon states.

  14. Magnetic dipole (M1) resonance Using the same interaction （and g’） as GTR analysis, RHAT can reproduce the excitation energy ! On the other hand, Exp.17.5 Strength is still overestimated though it is suppressed by the vacuum effect.

  15. π ν 1g9/2 1g9/2 2p1/2 2p3/2 2p1/2 1f5/2 2p3/2 1f7/2 1f5/2 π1f7/2 ν1f７/2 1f7/2 2s1/2 1d3/2 2s1/2 1d5/2 1d3/2 1d5/2 1p1/2 1p3/2 1p1/2 1p3/2 1s1/2 1s1/2 ＮＬ３ ＲＨＡＴ ＮＬ３ ＲＨＡＴ Shell structure for unstable nuclei 76Fe RHA + BCS calculation NL3: ΔE = -5.045 MeV (0.734) RHAT: ΔE = -6.382 MeV (0.710) 76Fe

  16. β-decay life times in 78Ni 78Ni T1/2= 2.0 sec (NL3) T1/2= 0.6 sec (RHAT) f0 Exp. T1/2~ 0.3 sec

  17. Summary • We have developed the calculation method of the vacuum polarization in relativistic Hartree approximation and fully-consistent RHA + RPA calculation using the derivative-expansion method. • The RHA calculation produces the enhanced effective mass naturally, because the inclusion of vacuum effect makes meson fields weak. • We have found that the relativistic effective mass is about 0.8 to reproduce the ISGQR excitation energies. • The quenching of the Gamow-Teller sum rule still remains with the vacuum polarization. In addition, we found the quenching of the M1 resonance caused by the vacuum polarization. • The inclusion of the vacuum polarization affects the shell structure around the Fermi level. As a result, the beta-decay life time in 78Ni is improved by this effect. The beta-decay and nuclear polarization analyses in unstable nucleus give us the evidence of the large effective mass, that is, a role of the vacuum polarization.

More Related