Dynamical tidal response of non-rotating relativistic stars

Understand

Accurately modeling the tidal response of neutron stars is crucial to connecting gravitational wave observations of binaries to ultra-dense nuclear physics.

• Most current models of the tidal response of relativistic stars either assume a static response model, or use phenomenological models inspired by Newtonian gravity.
• In this work, we present a general formalism for computing the linear dynamical tidal response function of relativistic, spherically symmetric stars.
• Our formalism incorporates stratification due to thermal and chemical imbalances, allowing one to study the effects of g modes on the tidal response function.