Speaker
Description
Neutron stars (NSs) experience internal oscillatory modes with characteristic frequencies that depend on their equation of state (EOS) and structure. Such modes can be resonantly excited during binary NS-BH/NS-NS inspirals, provided that the frequency of the tidal driving force exerted by the companion reaches the modes’ sufficiently before coalescence. These tidal resonances result in orbital energy being transferred to the modes, effectively reducing coalescing times and imprinting phase excesses on GW NS-NS or NS-BH inspirals [1, 2, 3]. In my talk at the LISA CosWG Meeting 2026, I can describe how accurate computations of NS modes impact multimessenger NS-NS/NS-BH observations physics of extremely dense matter (see, e.g., [4, 5]). As a first-year PhD student involved in the LISA CosWG 2026 local organizing committee, I will be happy to describe the work on GWs that is currently being carried out at the hosting institution, the Institut de Ciències del Cosmos de la Universitat de Barcelona (ICCUB), so as to help paving the way for the detection of NS resonances in future events observed by next-generation GW detectors. Our research involves computing NS modes based on EOS-informed models (using, e.g., pseudospectral collocation methods; see, e.g., [6]), calculating orbit-mode energy transfers (see Figure 1) that lead to reduced NS-NS/NS-BH coalescing times and estimating the detectability of resonance imprints in GW waveforms (see Figure 2).