MG12 - Talk detail
 

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 Participant 

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Abstract

Numerical and post-Newtonian estimates of tidal deformation in binary neutron stars

For most of the inspiral of a binary neutron star system, the stars are well-modeled as point particles. However, as they approach each other, an equation-of-state dependent tidal deformation modifies their orbits, changing the late inspiral waveform. The measurability of this effect in gravitational wave detectors can be estimated using both post-Newtonian tidal deformation calculations and full numerical simulations of binary neutron stars with varying equation of state. I will discuss the agreement and compatibility of these two methods.

Love numbers and tidal deformation for realistic neutron star equations of state

The tidal deformability of a neutron star is determined by the equation of state of matter within the star. During the early inspiral of a double neutron star binary, this deformability can be characterized by a single parameter, $\lambda$, related to the mass, radius, and Love numbers of the neutron stars. This parameter is determined by the equation of state for a given mass and mass ratio. I will discuss the calculation $\lambda$ for realistic neutron star equation of state tables, and the accuracy to which observations in advanced ground-based gravitational wave detectors could discriminate between candidate equations of state.

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