Tidal deformations of neutron stars with elastic crusts. (arXiv:2003.05449v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gittins_F/0/1/0/all/0/1">Fabian Gittins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andersson_N/0/1/0/all/0/1">Nils Andersson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pereira_J/0/1/0/all/0/1">Jonas P. Pereira</a>
With the first detections of binary neutron star mergers by
gravitational-wave detectors, it proves timely to consider how the internal
structure of neutron stars affects the way in which they can be asymmetrically
deformed. Such deformations may leave measurable imprints on gravitational-wave
signals and can be sourced through tidal interactions or the formation of
mountains. We detail the formalism that describes fully-relativistic neutron
star models with elastic crusts undergoing static perturbations. This formalism
primes the problem for studies into a variety of mechanisms that can deform a
neutron star. We present results for a barotropic equation of state and a
realistic model for the elastic crust, which enables us to compute relevant
quantities such as the tidal deformability parameter. We find that the
inclusion of an elastic crust provides a very small correction to the tidal
deformability. The results allow us to demonstrate when and where the crust
starts to fail during a binary inspiral and we find that the majority of the
crust will remain intact up until merger.
With the first detections of binary neutron star mergers by
gravitational-wave detectors, it proves timely to consider how the internal
structure of neutron stars affects the way in which they can be asymmetrically
deformed. Such deformations may leave measurable imprints on gravitational-wave
signals and can be sourced through tidal interactions or the formation of
mountains. We detail the formalism that describes fully-relativistic neutron
star models with elastic crusts undergoing static perturbations. This formalism
primes the problem for studies into a variety of mechanisms that can deform a
neutron star. We present results for a barotropic equation of state and a
realistic model for the elastic crust, which enables us to compute relevant
quantities such as the tidal deformability parameter. We find that the
inclusion of an elastic crust provides a very small correction to the tidal
deformability. The results allow us to demonstrate when and where the crust
starts to fail during a binary inspiral and we find that the majority of the
crust will remain intact up until merger.
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