Modelling neutron star mountains in relativity
Modelling neutron star mountains in relativity
Rapidly spinning, deformed neutron stars have long been considered potential gravitational-wave emitters. However, so far only upper limits on the size of the involved quadrupole deformations have been obtained. For this reason, it is pertinent to ask how large a mountain can be before the neutron star crust fractures. This is the question we consider in this paper, which describes how mountains can be calculated in relativistic gravity. Formally, this is a perturbative calculation that requires a fiducial force to source the mountain. Therefore, we consider three simple examples and increase their deforming amplitudes until the crust yields. We demonstrate how the derived mountains depend on the equation of state by considering a range of models obtained from chiral effective field theory. We find that the largest mountains depend sensitively on both the mechanism that sources them and the nuclear-matter equation of state.
gravitational waves, stars: neutron
116-128
Gittins, Fabian
657ec875-fac3-4606-9dcd-591ef22fc9f6
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
October 2021
Gittins, Fabian
657ec875-fac3-4606-9dcd-591ef22fc9f6
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Gittins, Fabian and Andersson, Nils
(2021)
Modelling neutron star mountains in relativity.
Monthly Notices of the Royal Astronomical Society, 507 (1), .
(doi:10.1093/mnras/stab2048).
Abstract
Rapidly spinning, deformed neutron stars have long been considered potential gravitational-wave emitters. However, so far only upper limits on the size of the involved quadrupole deformations have been obtained. For this reason, it is pertinent to ask how large a mountain can be before the neutron star crust fractures. This is the question we consider in this paper, which describes how mountains can be calculated in relativistic gravity. Formally, this is a perturbative calculation that requires a fiducial force to source the mountain. Therefore, we consider three simple examples and increase their deforming amplitudes until the crust yields. We demonstrate how the derived mountains depend on the equation of state by considering a range of models obtained from chiral effective field theory. We find that the largest mountains depend sensitively on both the mechanism that sources them and the nuclear-matter equation of state.
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Modelling neutron star mountains in relativity
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stab2048
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Accepted/In Press date: 14 July 2021
Published date: October 2021
Additional Information:
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Keywords:
gravitational waves, stars: neutron
Identifiers
Local EPrints ID: 454904
URI: http://eprints.soton.ac.uk/id/eprint/454904
ISSN: 1365-2966
PURE UUID: c90a1672-0118-48a0-be75-98c0093005ea
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Date deposited: 01 Mar 2022 17:42
Last modified: 17 Mar 2024 04:09
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Author:
Fabian Gittins
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