Formulating the r-mode Problem for Slowly Rotating Neutron Stars
Formulating the r-mode Problem for Slowly Rotating Neutron Stars
We revisit the problem of inertial r-modes in stratified stars, drawing on a more precise description of the
composition stratification in a mature neutron star. The results highlight issues with the traditional approach to the
problem, leading us to rethink the computational strategy for the r-modes of nonbarotropic neutron stars. We
outline two strategies for dealing with the problem. For moderate to slowly rotating neutron stars the only viable
alternative may be to approach the problem numerically from the outset, while a meaningful slow-rotation
calculation can be carried out for the fastest known spinning stars (which may be close to being driven unstable by
the emission of gravitational waves). We demonstrate that the latter approach leads to a problem close, but not
identical, to that for barotropic inertial modes. We also suggest that these reformulations of the problem likely
resolve the long-standing problem of singular behavior associated with a corotation point in rotating relativistic
neutron stars. This issue needs to be resolved in order to guide future gravitational-wave searches.
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Gittins, Fabian
657ec875-fac3-4606-9dcd-591ef22fc9f6
15 March 2023
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Gittins, Fabian
657ec875-fac3-4606-9dcd-591ef22fc9f6
Andersson, Nils and Gittins, Fabian
(2023)
Formulating the r-mode Problem for Slowly Rotating Neutron Stars.
The Astrophysical Journal, 945 (2), [139].
(doi:10.3847/1538-4357/acbc1e).
Abstract
We revisit the problem of inertial r-modes in stratified stars, drawing on a more precise description of the
composition stratification in a mature neutron star. The results highlight issues with the traditional approach to the
problem, leading us to rethink the computational strategy for the r-modes of nonbarotropic neutron stars. We
outline two strategies for dealing with the problem. For moderate to slowly rotating neutron stars the only viable
alternative may be to approach the problem numerically from the outset, while a meaningful slow-rotation
calculation can be carried out for the fastest known spinning stars (which may be close to being driven unstable by
the emission of gravitational waves). We demonstrate that the latter approach leads to a problem close, but not
identical, to that for barotropic inertial modes. We also suggest that these reformulations of the problem likely
resolve the long-standing problem of singular behavior associated with a corotation point in rotating relativistic
neutron stars. This issue needs to be resolved in order to guide future gravitational-wave searches.
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Accepted/In Press date: 13 February 2023
Published date: 15 March 2023
Additional Information:
Funding Information:
We acknowledge support from the STFC via grant No. ST/V000551/1. The contribution of N.A. was partly carried out at the Aspen Center for Physics, which is supported by a National Science Foundation grant No. PHY-1607611. He also thanks the Simons Foundation for generous travel support. The contribution of F.G. was partly carried out at the Institute for Nuclear Theory at the University of Washington during the “Neutron Rich Matter on Heaven and Earth” workshop, which is supported by the U.S. Department of Energy grant No. DE-FG02-00ER41132.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
Identifiers
Local EPrints ID: 476636
URI: http://eprints.soton.ac.uk/id/eprint/476636
ISSN: 0004-637X
PURE UUID: 59e2fa83-2005-49ac-98af-302634c46e5f
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Date deposited: 10 May 2023 16:48
Last modified: 17 Mar 2024 04:09
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Fabian Gittins
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