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Vorticity affects the stability of neutron stars

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Vorticity affects the stability of neutron stars. / Rezania, V.; Maartens, R.

In: Physical Review Letters, Vol. 84, No. 12, 20.03.2000, p. 2560-2563.

Research output: Contribution to journalArticlepeer-review

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Rezania, V & Maartens, R 2000, 'Vorticity affects the stability of neutron stars', Physical Review Letters, vol. 84, no. 12, pp. 2560-2563. https://doi.org/10.1103/PhysRevLett.84.2560

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Author

Rezania, V. ; Maartens, R. / Vorticity affects the stability of neutron stars. In: Physical Review Letters. 2000 ; Vol. 84, No. 12. pp. 2560-2563.

Bibtex

@article{e5318655965040269817b4d52a7df8e9,
title = "Vorticity affects the stability of neutron stars",
abstract = "The spin rate Ω of neutron stars at a given temperature T is constrained by the interplay between gravitational-radiation instabilities and viscous damping. Navier-Stokes theory has been used to calculate the viscous damping time scales and produce a stability curve for r modes in the (Ω,T ) plane. In Navier-Stokes theory, viscosity is independent of vorticity, but kinetic theory predicts a coupling of vorticity to the shear viscosity. We calculate this coupling and show that it can in principle significantly modify the stability diagram at lower temperatures. As a result, colder stars can remain stable at higher spin rates.",
author = "V. Rezania and R. Maartens",
year = "2000",
month = mar,
day = "20",
doi = "10.1103/PhysRevLett.84.2560",
language = "English",
volume = "84",
pages = "2560--2563",
journal = "Physical Review Letters",
issn = "0031-9007",
publisher = "American Physical Society",
number = "12",

}

RIS

TY - JOUR

T1 - Vorticity affects the stability of neutron stars

AU - Rezania, V.

AU - Maartens, R.

PY - 2000/3/20

Y1 - 2000/3/20

N2 - The spin rate Ω of neutron stars at a given temperature T is constrained by the interplay between gravitational-radiation instabilities and viscous damping. Navier-Stokes theory has been used to calculate the viscous damping time scales and produce a stability curve for r modes in the (Ω,T ) plane. In Navier-Stokes theory, viscosity is independent of vorticity, but kinetic theory predicts a coupling of vorticity to the shear viscosity. We calculate this coupling and show that it can in principle significantly modify the stability diagram at lower temperatures. As a result, colder stars can remain stable at higher spin rates.

AB - The spin rate Ω of neutron stars at a given temperature T is constrained by the interplay between gravitational-radiation instabilities and viscous damping. Navier-Stokes theory has been used to calculate the viscous damping time scales and produce a stability curve for r modes in the (Ω,T ) plane. In Navier-Stokes theory, viscosity is independent of vorticity, but kinetic theory predicts a coupling of vorticity to the shear viscosity. We calculate this coupling and show that it can in principle significantly modify the stability diagram at lower temperatures. As a result, colder stars can remain stable at higher spin rates.

UR - https://journals.aps.org/prl/issues/84/12

U2 - 10.1103/PhysRevLett.84.2560

DO - 10.1103/PhysRevLett.84.2560

M3 - Article

VL - 84

SP - 2560

EP - 2563

JO - Physical Review Letters

JF - Physical Review Letters

SN - 0031-9007

IS - 12

ER -

ID: 2870323