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Revealing the physics of r-modes in low-mass X-ray binaries

Revealing the physics of r-modes in low-mass X-ray binaries
Revealing the physics of r-modes in low-mass X-ray binaries
We consider the astrophysical constraints on the gravitational-wave driven r-mode instability in accreting neutron stars in low-mass X-ray binaries. We use recent results on superfluid and superconducting properties to infer the core temperature in these neutron stars and show the diversity of the observed population. Simple theoretical models indicate that many of these systems reside inside the r-mode instability region. However, this is in clear disagreement with expectations, especially for the systems containing the most rapidly rotating neutron stars. The inconsistency highlights the need to re-evaluate our understanding of the many areas of physics relevant to the r-mode instability. We summarize the current status of our understanding, and we discuss directions for future research which could resolve this dilemma.
101101-[5pp]
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Haskell, Brynmor
f2d24be8-4878-4ea0-9c90-21cb0e112c49
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Haskell, Brynmor
f2d24be8-4878-4ea0-9c90-21cb0e112c49

Ho, Wynn C.G., Andersson, Nils and Haskell, Brynmor (2011) Revealing the physics of r-modes in low-mass X-ray binaries. Physical Review Letters, 107, 101101-[5pp]. (doi:10.1103/PhysRevLett.107.101101).

Record type: Article

Abstract

We consider the astrophysical constraints on the gravitational-wave driven r-mode instability in accreting neutron stars in low-mass X-ray binaries. We use recent results on superfluid and superconducting properties to infer the core temperature in these neutron stars and show the diversity of the observed population. Simple theoretical models indicate that many of these systems reside inside the r-mode instability region. However, this is in clear disagreement with expectations, especially for the systems containing the most rapidly rotating neutron stars. The inconsistency highlights the need to re-evaluate our understanding of the many areas of physics relevant to the r-mode instability. We summarize the current status of our understanding, and we discuss directions for future research which could resolve this dilemma.

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Published date: 29 August 2011

Identifiers

Local EPrints ID: 194059
URI: http://eprints.soton.ac.uk/id/eprint/194059
PURE UUID: f8da5e57-cf5e-469b-8153-38f21f14cb4e
ORCID for Wynn C.G. Ho: ORCID iD orcid.org/0000-0002-6089-6836
ORCID for Nils Andersson: ORCID iD orcid.org/0000-0001-8550-3843

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Date deposited: 22 Jul 2011 15:35
Last modified: 28 Apr 2022 02:00

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Contributors

Author: Wynn C.G. Ho ORCID iD
Author: Nils Andersson ORCID iD
Author: Brynmor Haskell

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