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A rotational band with seven gamma-ray transitions between states with spin 2 Planck's constant and 16 Planck's constant has been observed in the doubly magic, self-conjugate nucleus (40)(20)Ca(20). The measured transition quadrupole moment of 1.80(+0.39)(-0.29)eb indicates a superdeformed shape with a deformation beta(2) = 0.59(+0.11)(-0.07). The features of this band are explained by cranked relativistic mean field calculations to arise from an 8-particle 8-hole excitation.

A candidate resonant tetraneutron state is found in the missing-mass spectrum obtained in the double-charge-exchange reaction ^{4}He(^{8}He,^{8}Be) at 186  MeV/u. The energy of the state is 0.83±0.65(stat)±1.25(syst)  MeV above the threshold of four-neutron decay with a significance level of 4.9σ. Utilizing the large positive Q value of the (^{8}He,^{8}Be) reaction, an almost recoilless condition of the four-neutron system was achieved so as to obtain a weakly interacting four-neutron system efficiently.

The electric dipole strength distribution in 120 Sn between 5 and 22 MeV has been determined at RCNP Osaka from polarization transfer observables measured in proton inelastic scattering at E0 = 295 MeV and forward angles including 0 • . Combined with photoabsorption data a highly precise electric dipole polarizability αD( 120 Sn) = 8.93(36) fm 3 is extracted. The dipole polarizability as isovector observable par excellence carries direct information on the nuclear symmetry energy and its density dependence. The correlation of the new value with the well established αD( 208 Pb) serves as a test of its prediction by nuclear energy density functionals (EDFs). Models based on modern Skyrme interactions describe the data fairly well while most calculations based on relativistic Hamiltonians cannot.PACS numbers: 21.10. Ky, 25.40.Ep, 21.60.Jz, 27.60.+j The nuclear equation of state (EOS) describing the energy of nuclear matter as function of its density has wide impact on nuclear physics and astrophysics [1] as well as physics beyond the standard model [2,3]. The EOS of symmetric nuclear matter with equal proton and neutron densities is well constrained from the ground state properties of finite nuclei, especially in the region of saturation density ρ 0 ≃ 0.16 fm −3 [4]. However, the description of astrophysical systems as, e.g., neutron stars requires knowledge of the EoS for asymmetric matter [5][6][7][8] which is related to the leading isovector parameters of nuclear matter, viz. the symmetry energy (J) and its derivative with respect to density (L) [9]. For a recent overview of experimental and theoretical studies of the symmetry energy see Ref. [10]. In spite of steady extension of knowledge on exotic nuclei, just these isovector properties are poorly determined by fits to experimental ground state data because the valley of nuclear stability is still extremely narrow along isotopic chains [11][12][13]. Thus one needs observables in finite nuclei specifically sensitive to isovector properties to better confine J and L. There are two such observables, the neutron skin r skin in nuclei with large neutron excess and the (static) dipole polarizability α D .The neutron skin thickness r skin = r n − r p defined as the difference of the neutron and proton root-meansquare radii r n,p is determined by the interplay between the surface tension and the pressure of excess neutrons on the core described by L [14,15]. Studies within nuclear density-funtional theory [16] show for all EDFs a strong correlation between r skin and the isovector symmetry energy parameters [17][18][19]. The most studied case so far is 208 Pb, where r skin has been derived from coherent photoproduction of π 0 mesons [20], antiproton annihilation [21,22], proton elastic scattering at 650 MeV [23] and 295 MeV [24], and from the dipole polarizability [25]. A nearly model-independent determination of the neutron skin is possible by measuring the weak form factor of nuclei with parity-violating elastic electron scattering [26]. Such an experiment has b...