Speaker
Description
This talk investigates the impact of assuming a barotropic equation of state (EoS) for neutron stars, which neglects potential out-of-β-equilibrium effects, on the calculation of oscillation modes. We focus on how the assumption of β-equilibrated EoS influences the frequencies of the non-radial fundamental (f) and first pressure (p1) modes. These calculations are performed using a wide set of neutron star models, each governed by different nucleonic EoS, generated through the metamodel technique. This framework integrates astrophysical observations, experimental nuclear physics, and chiral effective field theory. Additionally, we exploit quasi-universal relations to propose a method for estimating general relativity corrections to the commonly used Cowling approximation. Finally, we present a distribution of the expected f and p1 mode frequencies, which could be detectable by next-generation gravitational wave interferometers, offering new insights into neutron star structure.
