Neutron-star radii based on realistic nuclear interactions

Understand

The existence of neutron stars with $2M_\odot$ requires the strong stiffness of the equation of state (EoS) of neutron-star matter.

• We introduce a multi-pomeron exchange potential (MPP) working universally among 3- and 4-baryons to stiffen the EoS.
• Its strength is restricted by analyzing the nucleus-nucleus scattering with the G-matrix folding model.
• The EoSs are derived using the Brueckner-Hartree-Fock (BHF) and the cluster variational method (CVM) with the nuclear interactions ESC and AV18.