Elastic scattering on nucleons, νN → Nν, is the dominant supernova (SN) opacity source for μ and τ neutrinos. The dominant energyand number-changing processes were thought to be νe → eν and νν̄ ↔ ee until Suzuki (1993) showed that the bremsstrahlung process νν̄NN ↔ NN was actually more important. We find that for energy exchange, the related “inelastic scattering process” νNN ↔ NNν is even more e...

We study relationships between the neutron-rich skin of a heavy nucleus and the properties of neutron-star crusts. Relativistic effective field theories with a thicker neutron skin in 208Pb have a larger electron fraction and a lower liquid-to-solid transition density for neutron-rich matter. These properties are determined by the density dependence of the symmetry energy which we vary by addin...

Ground state properties of neutron rich even-even Be and C nuclei have been investigated using Relativistic Mean Field approach in co-ordinate space. The positions of the neutron drip line are correctly predicted for both the elements. The nucleus Be shows a two neutron halo but, contrary to expectation, C does not exhibit any halo structure. In carbon nuclei, N=16 comes out as a new magic numb...

Fast neutron scattering from natural lead was measured at the Rensselaer Polytechnic Institute’s (RPI) Gaerttner Linear Accelerator Center (LINAC). This measurement was performed using eight detectors positioned at different solid angles, with neutron events recorded in time of flight. This experiment used liquid scintillator EJ301 detectors and a tantalum photo-neutron target, which were optim...