Carlos Bertulani [NT/RBRC] Neutron skins and neutron stars

Friday 24 Apr 2026, 11:00 → 13:00 US/Eastern

CFNS Library (https://bnl.zoomgov.com/j/1614715193?pwd=WkwxODVWdzZzb29zQnZRVGp3VTBDQT09)

Neutron skins in stable and neutron-rich atomic nuclei are linked to the equation of state (EoS) of nuclear matter, which in turn influences the size, mass and, more generally, the internal structure of a neutron star. The thickness of this skin helps determine the nuclear symmetry energy, which is a crucial input for the EoS. I will report recent advances on theoretical and experimental methods to extract the symmetry energy of the EOS from nuclear reactions in the range of projectile energies range from  100 MeV/nucleon to several GeV/nucleon.