ÃÛÌÒTV

Abstract: During binary neutron star(BNS) inspiral, viscous processes in neutron star matter can damp out the tidal energy induced by the companion and heat up the star. Earlier investigations concluded that this tidal dissipation(or tidal heating) is negligible for neutron matter. But the cores of neutron stars reach densities several times the nuclear saturation density and could contain exotic particles such as hyperons and quarks. In this talk, I will demonstrate that the bulk viscosity originating from the non-leptonic weak interactions involving hyperons is several orders of magnitude higher than the standard neutron matter shear viscosity in the relevant temperature range of 0.001-0.1 MeV, and for heavier mass NSs (M≥1.6M⊙) that contain a significant fraction of hyperons in their core, the bulk viscosity can heat up the stars up to 0.1-1 MeV before the final merger. In principle, this can potentially be detected using future generation gravitational wave(GW) detectors. If not accounted for in BNS waveforms, this can also introduce systematic bias in tidal deformability estimation from GW observation and the equation of state inference. Lastly, I will present a scattering amplitude formalism to study this tidal heating effects of non-spinning neutron stars incorporating both worldline effective field theory and relativistic stellar perturbation theory.

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