Low-energy multipole response in nuclei at finite temperature

Low-energy multipole response in nuclei at finite temperature

Y. F. Niu N. Paar D. Vretenar J. Meng Physics Department, Faculty of Science, University of Zagreb, Croatia State Key Laboratory for Nuclear Physics and Technology, School of Physics, Peking University, Beijing 100871, China School of Physics and Nuclear Energy, Beihang University, Beijing 100083, China

The multipole response of nuclei at temperatures MeV is studied using a self-consistent finite-temperature RPA (random phase approximation) based on relativistic energy density functionals. Illustrative calculations are performed for the isoscalar monopole and isovector dipole modes and, in particular, the evolution of low-energy excitations with temperature is analyzed, including the modification of pygmy structures. Both for the monopole and dipole modes, in the temperature range MeV additional transition strength appears at low energies because of thermal unblocking of single-particle orbitals close to the Fermi level. A concentration of dipole strength around 10 MeV excitation energy is predicted in Ni, where no low-energy excitations occur at zero temperature. The principal effect of finite temperature on low-energy strength that is already present at zero temperature, e.g. in Ni and Sn, is the spreading of this structure to even lower energy and the appearance of states that correspond to thermally unblocked transitions.

hot nuclei, pygmy resonances, giant resonances, random phase approximation
21.10.Gv, 21.30.Fe, 21.60.Jz, 24.30.Cz
journal: Physics Letters B

The multipole response of nuclei at energies close to the neutron emission threshold, and the possible occurrence of exotic low-energy modes of excitation, present a rapidly growing field of research PVKC.07 (). For instance, in nuclei with a pronounced neutron excess, the phenomenon of pygmy dipole resonance (PDR), a low-energy mode that corresponds to oscillations of a weakly-bound neutron skin against the isospin saturated proton-neutron core, has been analyzed in a number of experimental and theoretical studies. In particular, recent and experiments Sav.06 (); Sch.08 (); Oze.08 () have disclosed interesting features of the concentration of low-energy electric-dipole excitations. Exotic nuclear dynamics has also been explored in experiments with radioactive ion beams, extending the studies of low-lying dipole response toward nuclei with more pronounced neutron excess Adr.05 (); Wie.09 ().

Features of PDR in medium-heavy and heavy nuclei place constraints on the nuclear matter symmetry energy, and can also provide information on the size of the neutron skin Pie.06 (); Kli.07 (). A concentration of electric-dipole strength at low energy is interesting not only as a unique structure phenomenon, but it could also play an important role in astrophysical processes. For instance, it could affect neutron capture rates in r-process nucleosynthesis Gor.98 (); Lit.09 (). Reactions relevant for the r-process take place in stellar environment at finite temperature. Calculations of neutron capture rates on neutron-rich nuclei have typically included temperature only as a parameter of the Lorentzian function used to fold the E1 strength distribution Gor.98 (); Gor.02 (). It would, of course, be useful to perform these calculations using a microscopic framework that provides a consistent description of nuclear ground-state properties and excitations at finite temperature. In particular, temperature induced modifications of low-energy dipole strength close to the neutron separation energy, e.g the thermal unblocking of additional transitions, should be described in a consistent theoretical framework.

In this work we introduce a fully self-consistent finite-temperature RPA (random phase approximation) framework based on relativistic energy density functionals, and explore the evolution of multipole response as a function of temperature. The goal is to analyze how low-energy excitations evolve with temperature, the modification of the structure of PDR, and the possible occurrence of excitation modes that are not present in nuclei at zero temperature.

The multipole response of hot nuclei has been studied using a variety of theoretical approaches, including e.g. the RPA based on schematic interactions Civ.84 (); Vau.84 (); Bes.84 (), linear response theory Fab.83 (); Rin.84 (), Hartree-Fock plus RPA with Skyrme effective interactions Sag.84 (), RPA models extended with the inclusion of collision terms Lac.98 (). The decay of hot nuclei and thermal damping of giant resonances have also been explored in numerous studies, e.g. in Refs. Gal.85 (); Bor.86 (); Dan.96 (); OBA.96 (); Dan.97 (); Lar.99 (); Sto.04 (), as well as sum rules at finite temperature Mey.83 (); Bar.85 (). Finite temperature Hartree-Fock Bogoliubov (HFB) theory Goo.81 () has been used as the basis for the corresponding quasiparticle RPA Som.83 (); Kha.04 (). Experimental studies of giant resonances in hot nuclei are carried out by measuring high energy -rays from the decay of resonant states built on excited states of target nuclei Bra.89 (); Tve.96 (); Pie.96 (); Bau.98 ().

The self-consistent finite temperature relativistic random phase approximation (FTRRPA) is formulated in the single-nucleon basis of the relativistic mean-field (RMF) model at finite temperature (FTRMF). This model has been introduced in Ref. Gam.00 (), based on the nonlinear Lagrangian NL3 LKR.97 (). In the theoretical framework that we use in the present analysis relativistic effective interactions are implemented self-consistently, i.e., both the FTRMF equations and the matrix equations of FTRRPA are based on the same relativistic energy density functional with medium-dependent meson-nucleon couplings NVFR.02 (). Of course, the description of open-shell nuclei necessitates a consistent treatment of pairing correlations like, for instance, in the finite temperature HFB+QRPA framework Som.83 (). However, in nuclei the phase transition from a superfluid to a normal state occurs at temperatures MeV Goo.81 (); Kha.04 (), whereas for temperatures above MeV contributions from states in the continuum become large, and additional subtraction schemes have to be implemented to remove the contributions of the external nucleon gas Bon.84 (). Therefore, we consider the temperatures in the range MeV, for which the FTRMF plus FTRRPA should provide an accurate description of the evolution of multipole response.

The FTRRPA represents the small amplitude limit of the time-dependent relativistic mean-field theory at finite temperature. Starting from the response of the time-dependent density matrix to an external field , the equation of motion for the density operator reads


In the small amplitude limit the density matrix is expanded to linear order


where denotes the stationary ground-state density.


and includes the thermal occupation factors of single-particle states . The resulting FTRRPA equations read






The RRPA matrices A and B are composed of matrix elements of the residual interaction , derived from an effective Lagrangian density with medium-dependent meson-nucleon couplings NVFR.02 (), as well as certain combinations of thermal occupation factors . The diagonal matrix elements contain differences of single particle energies , where . Because of finite temperature, the configuration space includes particle-hole (), particle-particle (), and hole-hole () pairs. In addition to configurations of positive energy, the FTRRPA configuration space must also contain pair-configurations formed from the fully or partially occupied states of positive energy and the empty negative-energy states from the Dirac sea. The inclusion of configurations built from occupied positive-energy states and empty negative-energy states is essential for current conservation, decoupling of spurious states, and for a quantitative description of excitation energies of giant resonances PRNV.03 ().

The residual interaction is derived from the DD-ME2 effective Lagrangian LNVR.05 (), and single-particle occupation factors at finite temperature are included in a consistent way both in the FTRMF and FTRRPA. The same interaction is used both in the FTRMF equations that determine the single-nucleon basis, and in the matrix equations of the FTRRPA. The full set of FTRRPA equations is solved by diagonalization. The result are excitation energies , and the corresponding forward- and backward-going amplitudes and , respectively, that are used to evaluate the transition strength for a multipole operator :


Discrete spectra are averaged with a Lorentzian distribution of arbitrary width ( MeV in the present calculation).

In Fig. 1 we display the FTRRPA strength distributions in Ni, Zr, Sn, and Pb for the isoscalar monopole operator, at temperatures , and 2 MeV. At zero temperature the transition strength distributions are clearly dominated by the pronounced collective isoscalar giant monopole resonance (ISGMR). Even by increasing the temperature to MeV, the ISGMR gets only slightly modified in Zr, Sn, and Pb. In the lighter nucleus Ni, where the ISGMR is less collective and therefore more sensitive to modifications of the corresponding configuration space at finite temperature, at MeV the overall strength distribution is lowered by MeV. It is interesting to note that for all nuclei under consideration, in the temperature range MeV additional transition strength appears at energies below 10 MeV. These low-energy transitions occur because of thermal unblocking of single-particle orbitals close to the Fermi level. The effect of finite temperature is especially pronounced for the neutron-rich nucleus Sn, due to transitions from thermally populated weakly-bound neutron orbits. The low-energy strength is dominated by two rather pronounced peaks. The state at 5.45 MeV corresponds to the single-neutron transition from thermally unblocked orbitals: 3p 4p, whereas for the state at 7.02 MeV the dominant transition is between the neutron orbitals 2f and 3f.

As already emphasized in the introduction, particularly relevant for possible astrophysical applications is a microscopic description of low-energy dipole response in hot nuclei. Fig. 2 displays the FTRRPA (DD-ME2) dipole strength distributions in Ni isotopes, at temperatures , and 2 MeV. The transition matrix elements are evaluated for the isovector dipole operator. At zero temperature the main peak of the isovector giant dipole resonance (IVGDR) is located at  18 MeV. For Ni, in particular, additional low-energy PDR structure is predicted below 10 MeV even at zero temperature, and this result was recently confirmed in the experimental study reported in Ref. Wie.09 (). The IVGDR is somewhat modified at finite temperature. At MeV the main peak is lowered by MeV in Ni, whereas in Ni finite temperature reduces the fragmentation of the IVGDR strength in the interval 17-20 MeV, and enhances the collectivity of the main resonance peak.

A very interesting finite temperature effect is predicted for the dipole strength distributions of Ni, where no low-energy excitations are present at zero temperature. Already at MeV novel transition strength develops below 10 MeV. For Ni, in particular, at MeV the main low-energy peak is located at 9.71 MeV, it exhausts 1.54% of the Thomas Reiche Kuhn(TRK) sum rule, and is composed of 5 neutron and 4 proton single-particle transitions: (45.87%), (13.92%), (8.43%), (3.58%), (1.30%), (7.89%), (6.32%), (3.62%), and (1.21%). The percentage in brackets corresponds to the contribution of a particular transition to the total FTRRPA amplitude for the state at 9.71 MeV. This rather rich RPA structure shows that the new low-energy state accumulates a small degree of collectivity due to thermal population of both neutron and proton single-particle levels around the Fermi surface.

In the case of Ni, two pronounced low-energy peaks are calculated at temperature MeV: the states at 9.78 MeV and 10.03 MeV, exhausting 1.2% and 1.5% of the TRK sum rule, respectively. It is interesting to note that both states are dominated by proton transitions. For the state at 9.78 MeV: (48.02%), (20.99%), (3.12%), (17.06%), (4.36%), and (1.22%). The structure of the state at 10.03 MeV appears to be less distributed, i.e. it is dominated by the transitions (26.55%), (3.59%), (63.60%), and (2.55%).

In Ni, where the PDR structure is present already at , the increase in temperature leads to fragmentation of the PDR and its spreading to even lower energy. These examples nicely illustrate the variety of effects one can expect for the dipole response of hot nuclei, e.g. the appearance of novel modes of low-energy excitations dominated by proton transitions, and the thermal spreading of PDR structures in neutron-rich nuclei.

Finally, Fig. 3 shows the evolution of FTRRPA dipole transition strength with temperature for Sn. This is an important example, because for this nucleus the occurrence of PDR was predicted in several theoretical studies PVKC.07 (), and recently confirmed in Coulomb dissociation experiments Adr.05 (). With the increase of temperature up to MeV the transition strength is virtually unchanged. Higher temperatures, however, have a pronounced effect on low-energy dipole strength. At temperatures MeV, even though the main PDR peak at MeV does not change much, additional low-energy single-particle transitions appear in the interval MeV: E=3.75 MeV, (99.65%); E=4.54 MeV, (97.49%); E=4.92 MeV, (99.58%); E=6.12 MeV, (98.35%). At zero temperature the PDR state is calculated at MeV, whereas at MeV the PDR excitation energy is MeV. In Table 1 we compare the structure of FTRRPA states for the main PDR peaks at temperatures MeV and MeV. The amplitudes of transitions dominant at MeV get slightly reduced at higher temperature. Because of thermal unblocking of the orbit, at MeV an additional non-negligible contribution to the PDR peak corresponds to the transition 1g 1h.

51.85 50.37
19.15 17.22
11.56 10.43
6.64 5.48
4.99 4.44
2.17 2.43
- 1.26
Table 1: FTRRPA transition amplitudes for the main PDR peaks in Sn at temperatures MeV and MeV. Included are the contributions (in %) of dominant configuration to the total sum of FTRRPA amplitudes: .

The results for the evolution of dipole response with temperature (c.f. Figs. 2 and 3) show that the principal effect of finite temperature on low-energy strength that is already present at zero temperature, e.g. in Ni and Sn, is the spreading of this structure to even lower energy and the appearance of states that correspond to thermally unblocked transitions. This could be important for calculation of astrophysical neutron capture rates relevant for r-process nucleosynthesis, because these reactions take place at finite temperature. As recently pointed out in Ref. Lit.09 (), neutron capture rates computed with the Hauser-Feshbach model are sensitive to the fine structure of low-energy dipole transitions, emphasizing the importance of reliable microscopic predictions for the evolution of PDR structures both with neutron number and nuclear temperature.

This work was supported by the Unity through Knowledge Fund (UKF Grant No. 17/08) and MZOS - project 1191005-1010. Y. F. Niu acknowledges support from the Croatian National Foundation for Science, Higher Education and Technological Development. The work of J.M and D.V. was supported in part by the Chinese-Croatian project “Nuclear structure far from stability”.


  • (1) N. Paar, D. Vretenar, E. Khan, and G. Colò, Rep. Prog. Phys. 70 (2007) 691
  • (2) D. Savran, M. Babilon, A. M. van den Berg, M. N. Harakeh, J. Hasper, A. Matic, H. J. Wörtche, and A. Zilges, Phys. Rev. Lett. 97 (2006) 172502
  • (3) R. Schwengner, G. Rusev, N. Tsoneva, et al., Phys. Rev. C 78 (2008) 064314
  • (4) B. Özel, J. Enders, H. Lenske, et al., arXiv:0901.2443v1
  • (5) P. Adrich, A. Klimkiewicz, M. Fallot, et al., Phys. Rev. Lett. 95 (2005) 132501
  • (6) O. Wieland, A. Bracco, F. Camera, et. al., Phys. Rev. Lett. 102 (2009) 092502
  • (7) J. Piekarewicz, Phys. Rev. C 73 (2006) 044325
  • (8) A. Klimkiewicz et al., Phys. Rev. C 76 (2007) 051603(R)
  • (9) S. Goriely, Phys. Lett. B 436 (1998) 10
  • (10) E. Litvinova et al., Nucl. Phys. A 823 (2009) 26
  • (11) S. Goriely, E. Khan, Nucl. Phys. A 706 (2002) 217
  • (12) O. Civitarese, R. A. Broglia, and C. H. Dasso, Ann. Phys. 156 (1984) 142
  • (13) D. Vautherin and N. Vinh Mau, Nucl. Phys. A 422 (1984) 140
  • (14) W. Besold, P.-G. Reinhard, and C. Toepffer, Nucl. Phys. A 431 (1984) 1
  • (15) M. E. Faber, J. L. Egido, and P. Ring, Phys. Lett. B 127 (1983) 5
  • (16) P. Ring, L. M. Robledo, J. L. Egido, and M. Faber, Nucl. Phys. A 419 (1984) 261
  • (17) H. Sagawa and G. F. Bertsch, Phys. Lett. B 146 (1984) 138
  • (18) D. Lacroix, P. Chomaz, and S. Ayik, Phys. Rev. C 58 (1998) 2154
  • (19) M. Gallardo, M. Diebel, T. Dossing, and R. A. Broglia, Nucl. Phys. A 443 (1985) 415
  • (20) P. F. Bortignon, R. A. Broglia, G. F. Bertsch, and J. Pacheco, Nucl. Phys. A 460 (1986) 149
  • (21) N. D. Dang, Phys. Rep. 264 (1996) 123
  • (22) W. E. Ormand, P. F. Bortignon, and R. A. Broglia, Phys. Rev. Lett. 77 (1996) 607
  • (23) Nguyen Dinh Dang and Fumihiko Sakata, Phys. Rev. C 55 (1997) 2872
  • (24) A. B. Larionov, M. Cabibbo, V Baran, and M. Di Toro, Nucl. Phys. A 648 (1999) 157
  • (25) A. N. Storozhenko, A. I. Vdovin, A. Ventura, and A. I. Blokhin, Phys. Rev. C 69 (2004) 064320
  • (26) J. Meyer, P. Quentin, and M. Brack, PHys. Lett. B 133 (1983) 279
  • (27) M. Barranco, A. Polls, and J. Martorell, Nucl. Phys. A 444 (1985) 445
  • (28) A. L. Goodman, Nucl. Phys. A 352 (1981) 30
  • (29) H. M. Sommermann, Ann. Phys. 151 (1983) 163
  • (30) E. Khan, Nguyen Van Giai, and M. Grasso, Nucl. Phys. A 731 (2004) 311
  • (31) A. Bracco et al., Phys. Rev. Lett. 62 (1989) 2080
  • (32) T. S. Tveter et al., Phys. Rev. Lett. 76 (1996) 1035
  • (33) D. Pierroutsakou et al., Nucl. Phys. A 600 (1996) 131
  • (34) T. Baumann et al., Nucl. Phys. A 635 (1998) 428
  • (35) Y. K. Gambhir, J. P. Maharana, G. A. Lalazissis, C. P. Panos, and P. Ring, Phys. Rev. C 62 (2000) 054610
  • (36) G.A. Lalazissis, J. König, and P. Ring, Phys. Rev. C 55, (1997) 540
  • (37) T. Nikšić, D. Vretenar, P. Finelli, P. Ring, Phys. Rev. C 66 (2002) 024306
  • (38) P. Bonche, S. Levit, and D. Vautherin, Nucl. Phys. A 427 (1984) 278
  • (39) N. Paar, P. Ring, T. Nikšić, and D. Vretenar, Phys. Rev. C 67 (2003) 034312
  • (40) G. A. Lalazissis, T. Nikšić, D. Vretenar, and P. Ring, Phys. Rev. C 71 (2005) 024312
Figure 1: Isoscalar monopole transition strength distributions in Ni, Zr, Sn, and Pb, calculated with the FTRRPA (DD-ME2) at temperatures , and 2 MeV.
Figure 2: Isovector dipole strength distributions in Ni isotopes at temperatures , and 2 MeV, calculated with the FTRRPA (DD-ME2).
Figure 3: Evolution of electric dipole transition strength with temperature in Sn, calculated with the FTRRPA (DD-ME2).
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