Neutron-star tidal deformability and equation-of-state constraints
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Neutron-star tidal deformability and equation-of-state constraints Katerina Chatziioannou1 Received: 18 May 2020 / Accepted: 9 October 2020 © Springer Science+Business Media, LLC, part of Springer Nature 2020
Abstract Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin asymmetry, uniquely determine the stars’ macroscopic properties within General Relativity. Astrophysical constraints on those macroscopic properties, such as neutron-star masses and radii, have long been used to understand the microscopic properties of the matter that forms them. In this article we discuss another astrophysically observable macroscopic property of neutron stars that can be used to study their interiors: their tidal deformation. Neutron stars, much like any other extended object with structure, are tidally deformed when under the influence of an external tidal field. In the context of coalescences of neutron stars observed through their gravitational-wave emission, this deformation, quantified through a parameter termed the tidal deformability, can be measured. We discuss the role of the tidal deformability in observations of coalescing neutron stars with gravitational waves and how it can be used to probe the internal structure of Nature’s most compact matter objects. Perhaps inevitably, a large portion of the discussion will be dictated by GW170817, the most informative confirmed detection of a binary neutron-star coalescence with gravitational waves as of the time of writing. Keywords Binary neutron stars · Coalescence · Tidal deformation
This article belongs to a Topical Collection: Binary Neutron Star mergers.
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Katerina Chatziioannou [email protected] Center for Computational Astrophysics, Flatiron Institute, 162 5th Ave, New York, NY 10010, USA 0123456789().: V,-vol
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Contents 1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2 The tidal deformation of a compact object . . . . . . . . . . . . . . . . . 2.1 The neutron-star tidal deformability . . . . . . . . . . . . . . . . . 2.2 Computing the tidal deformability . . . . . . . . . . . . . . . . . . 2.3 Beyond the tidal deformability . . . . . . . . . . . . . . . . . . . . 2.4 The tidal deformability of a black hole . . . . . . . . . . . . . . . . 3 Measuring the tidal deformability with neutron-star coalescences . . . . 3.1 The gravitational-wave phase . . . . . . . . . . . . . . . . . . . . . 3.2 Tidal constraints and inference on the equation of state . . . . . . . 3.2.1 Measurement accuracy for tidal parameters . . . . . . . . . . 3.2.2 Measuring the tidal deformability and radius of a neutron star 3.2.3 Combining information from multiple signals . . . . . . . . . 3.2.4 Effect of the mass distribution and other population parameters 3.2.5 Non gravitational-wave messengers . . . . . . . . .
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