The first excited 0(+) state in 12C (Hoyle state) has been predicted to be a dilute self-bound gas of bosonic alpha particles, similar to a Bose-Einstein condensate. To clarify this conjecture, precise electron scattering data on form factors of the ground state and the transition to the Hoyle state are compared with results of the fermionic molecular dynamics model, a microscopic alpha-cluster model, and an alpha-cluster model with reduced degrees of freedom (in the spirit of a Bose-Einstein condensed state). The data indicate clearly a dilute density with a large spatial extension of the Hoyle state. A closer inspection of the model calculations, which reproduce the experimental findings, reveals that the term Bose-Einstein condensation of three alpha particles must not be taken too literally.

A benchmark experiment on (208)Pb shows that polarized proton inelastic scattering at very forward angles including 0° is a powerful tool for high-resolution studies of electric dipole (E1) and spin magnetic dipole (M1) modes in nuclei over a broad excitation energy range to test up-to-date nuclear models. The extracted E1 polarizability leads to a neutron skin thickness r(skin) = 0.156(-0.021)(+0.025) fm in (208)Pb derived within a mean-field model [Phys. Rev. C 81, 051303 (2010)], thereby constraining the symmetry energy and its density dependence relevant to the description of neutron stars.

The nucleus is one of the most multi-faceted many-body systems in the universe. It exhibits a multitude of responses depending on the way one 'probes' it. With increasing technical advancements of beams at the various accelerators and of detection systems the nucleus has, over and over again, surprised us by expressing always new ways of 'organized' structures and layers of complexity. Nuclear magnetism is one of those fascinating faces of the atomic nucleus we discuss in the present review. We shall not just limit ourselves to presenting the by now very large data set that has been obtained in the last two decades using various probes, electromagnetic and hadronic alike and that presents ample evidence for a low-lying orbital scissors mode around 3 MeV, albeit fragmented over an energy interval of the order of 1.5 MeV, and higher-lying spin-flip strength in the energy region 5 − 9 MeV in deformed nuclei, nor to the presently discovered evidence for low-lying proton-neutron isovector quadrupole excitations in spherical nuclei. To the contrary, we put the experimental evidence in the perspectives of understanding the atomic nucleus and its various structures of well-organized modes of motion and thus enlarge our discussion to more general fermion and bosonic many-body systems.

A high-resolution (gamma,gamma') study of the electric dipole response in 208Pb at the S-DALINAC reveals a resonance structure centered around the neutron emission threshold. Microscopic quasiparticle phonon model calculations in realistic model spaces including the coupling to complex configurations are able to describe the data in great detail. The resonance is shown to result from surface density oscillations of the neutron skin relative to an approximately isospin-saturated core. It also forms an integral part of a toroidal E1 mode representing an example of vortex collective motion in nuclei.

The electric dipole strength distribution in 48 Ca between 5 and 25 MeV has been determined at RCNP, Osaka, from proton inelastic scattering experiments at forward angles. Combined with photoabsorption data at higher excitation energy, this enables the first extraction of the electric dipole polarizability αD( 48 Ca) = 2.07(22) fm 3 . Remarkably, the dipole response of 48 Ca is found to be very similar to that of 40 Ca, consistent with a small neutron skin in 48 Ca. The experimental results are in good agreement with ab initio calculations based on chiral effective field theory interactions and with state-of-the-art density-functional calculations, implying a neutron skin in 48 Ca of 0.14 − 0.20 fm.Introduction.-The equation of state (EOS) of neutronrich matter governs the properties of neutron-rich nuclei, the structure of neutron stars, and the dynamics of corecollapse supernovae [1,2]. The largest uncertainty of the EOS at nuclear densities for neutron-rich conditions stems from the limited knowledge of the symmetry energy J, which is the difference of the energies of neutron and nuclear matter at saturation density, and the slope of the symmetry energy L, which is related to the pressure of neutron matter. The symmetry energy also plays an important role in nuclei, where it contributes to the formation of neutron skins in the presence of a neutron excess. Calculations based on energy density functionals (EDFs) pointed out that J and L can be correlated with isovector collective excitations of the nucleus such as pygmy dipole resonances [3] and giant dipole resonances (GDRs) [4], thus suggesting that the neutron skin thickness, the difference of the neutron and proton root-mean-square radii, could be constrained by studying properties of collective isovector observables at low energy [5]. One such observable is the nuclear electric dipole polarizability α D , which represents a viable tool to constrain the EOS of neutron matter and the physics of neutron stars [6][7][8][9][10][11].While correlations among α D , the neutron skin and the symmetry energy parameters have been studied extensively with EDFs [12][13][14][15][16], only recently have ab initio calculations based on chiral effective field theory (χEFT) interactions successfully studied such correlations in medium-mass nuclei [17,18]. By using a set of chiral two-plus three-nucleon interactions [19,20] and

Scattering of protons of several hundred MeV is a promising new spectroscopic tool for the study of electric dipole strength in nuclei. A case study of 208 Pb shows that at very forward angles J π = 1 − states are strongly populated via Coulomb excitation. A separation from nuclear excitation of other modes is achieved by a multipole decomposition analysis of the experimental cross sections based on theoretical angular distributions calculated within the quasiparticle-phonon model. The B(E1) transition strength distribution is extracted for excitation energies up to 9 MeV, i.e., in the region of the so-called pygmy dipole resonance (PDR). The Coulomb-nuclear interference shows sensitivity to the underlying structure of the E1 transitions, which allows for the first time an experimental extraction of the electromagnetic transition strength and the energy centroid of the PDR.

Spectra of the 9 Be(e,e) reaction have been measured at the Superconducting Darmstadt Electron Linear Accelerator at an electron energy of E 0 = 73 MeV and scattering angles of 93 • and 141 • with high-energy resolution up to excitation energies of E x = 8 MeV. The astrophysically relevant resonance parameters of the first excited 1/2 + state of 9 Be have been extracted in a one-level approximation of R-matrix theory, resulting in resonance energy E R = 1.748(6) MeV and width R = 274(8) keV, which are in good agreement with the latest 9 Be(γ ,n) experiment but with considerably improved uncertainties. However, the reduced B(E1) transition strength deduced from an extrapolation of the (e,e) data to the photon point is smaller by a factor of two. Implications of the new results for possible production of 12 C in neutron-rich astrophysical scenarios are discussed.

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...