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• W2578955122 abstract "A principal goal of gravitational-wave astronomy is to constrain the neutron star equation of state (EOS) by measuring the tidal deformability of neutron stars. The tidally induced departure of the waveform from that of a point particle [or a spinless binary black hole (BBH)] increases with the stiffness of the EOS. We show that causality (the requirement that the speed of sound be less than the speed of light for a perfect fluid satisfying a one-parameter equation of state) places an upper bound on tidal deformability as a function of mass. Like the upper mass limit, the limit on deformability is obtained by using an EOS with ${v}_{text{sound}}=c$ for high densities and matching to a low density (candidate) EOS at a matching density of order nuclear saturation density. We use these results and those of Lackey et al. [Phys. Rev. D 89, 043009 (2014)] to estimate the resulting upper limit on the gravitational-wave phase shift of a black hole--neutron star (BHNS) binary relative to a BBH. Even for assumptions weak enough to allow a maximum mass of $4text{ }text{ }{M}_{ensuremath{bigodot}}$ (a match at nuclear saturation density to an unusually stiff low-density candidate EOS), the upper limit on dimensionless tidal deformability is stringent. It leads to a still more stringent estimated upper limit on the maximum tidally induced phase shift prior to merger. We comment in an appendix on the relation among causality, the condition ${v}_{text{sound}}<c$, and the condition $dp/densuremath{epsilon}<1$ for the effective EOS governing the equilibrium star." @default.
• W2578955122 created "2017-01-26" @default.
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• W2578955122 date "2017-04-27" @default.
• W2578955122 modified "2023-10-15" @default.
• W2578955122 title "Upper limit set by causality on the tidal deformability of a neutron star" @default.
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• W2578955122 doi "https://doi.org/10.1103/physrevd.95.083014" @default.
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