Program

This workshop aims at stimulating collaborations and fertilize the dialog between the nuclear physics and the astrophysics communities in the quest to determine the properties of the dense matter equation of state. On the one hand, efforts in the microscopic description of neutron-rich matter can help to constrain and to validate the large number of equations of state (EoSs) employed in astrophysical numerical simulations. On the other hand, neutron-star oscillations produced in astrophysical events such as core-collapse supernovae or neutron-star mergers represent a unique probe for high-density matter. Numerical calculations which simulate such events, indicate strong correlations between the characteristic oscillation frequencies and the employed EoS. The characteristic oscillations are visible in the gravitational-wave signal and may be measurable as the sensitivity of the current instruments increases. Moreover, the late inspiral phase of double neutron star binaries and of neutron star-black hole binaries exhibits finite-size effects, and the corresponding gravitational-wave signal can reveal the stellar tidal deformability and thus EoS properties. Hence, an interplay between gravitational-wave astronomy, together with astrophysical simulations and input from nuclear physics, could finally help to pin down the dense matter EoS.