Speaker
Description
Neutron-rich matter exists naturally in neutron stars and neutron skins of heavy nuclei. It can also be created during mergers of neutron stars in space and heavy-ion collisions in terrestrial laboratories. The Equation of State (EOS) of such matter is still very poorly known but has broad impacts on many interesting issues in both astrophysics and nuclear physics. In particular, nuclear symmetry energy encoding the energy cost to make the nuclear matter more neutron-rich has been the most uncertain part of the EOS of dense neutron-rich nucleonic matter. It affects the masses, radii, tidal deformations, cooling rates, and frequencies of various oscillation modes of isolated neutron stars as well as the strain amplitude and frequencies of gravitational waves from neutron star mergers.
In this talk, we will discuss the interplay and effects of neutron skins and short-range nucleon-nucleon correlations in the initial state of colliding nuclei and the density dependence of nuclear symmetry energy on observables of heavy-ion reactions from FRIB to FAIR energies.
| What kind of work does this abstract pertain to? | Theoretical |
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| Which experiment is this abstract related to? | Other |
