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Volumn 86, Issue 7, 2001, Pages 1152-1155

Nonlinear evolution of the r-modes in neutron stars

Author keywords

[No Author keywords available]

Indexed keywords

GRAVITATIONAL RADIATION; NEUTRON STARS; NEWTONIAN EQUATIONS; ROTATIONAL KINETIC ENERGY;

EID: 14344281052     PISSN: 00319007     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevLett.86.1152     Document Type: Article
Times cited : (104)

References (20)
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    • preceding Letter
    • N. Stergioulas and J. A. Font, preceding Letter, Phys. Rev. Lett. 86, 1148 (2001), evolve relativistic fluids in the Cowling approximation without GR reaction and find no r-mode saturation at unit amplitude.
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  • 8
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    • K. C. B. New and J. E. Tohline, Astrophys. J. 490, 311 (1997); H. S. Cohl and J. E. Tohline, Astrophys. J. 527, 527 (1999); J. E. Cazes and J. E. Tohline, Astrophys. J. 532, 1051 (2000).
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    • K. C. B. New and J. E. Tohline, Astrophys. J. 490, 311 (1997); H. S. Cohl and J. E. Tohline, Astrophys. J. 527, 527 (1999); J. E. Cazes and J. E. Tohline, Astrophys. J. 532, 1051 (2000).
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  • 10
    • 0034164197 scopus 로고    scopus 로고
    • K. C. B. New and J. E. Tohline, Astrophys. J. 490, 311 (1997); H. S. Cohl and J. E. Tohline, Astrophys. J. 527, 527 (1999); J. E. Cazes and J. E. Tohline, Astrophys. J. 532, 1051 (2000).
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    • Cazes, J.E.1    Tohline, J.E.2
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    • note
    • 22.
  • 13
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    • H. Spruit, Astron. Astrophys. 341, L1 (1999); L. Rezzolla, F. K. Lamb, and S. L. Shapiro, Astrophys. J. 531, L139 (2000); Y. Levin and G. Ushomirsky, Mon. Not. R. Astron. Soc. (to be published); W. C. G. Ho and D. Lai, Astrophys. J. (to be published).
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    • Spruit, H.1
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    • H. Spruit, Astron. Astrophys. 341, L1 (1999); L. Rezzolla, F. K. Lamb, and S. L. Shapiro, Astrophys. J. 531, L139 (2000); Y. Levin and G. Ushomirsky, Mon. Not. R. Astron. Soc. (to be published); W. C. G. Ho and D. Lai, Astrophys. J. (to be published).
    • (2000) Astrophys. J. , vol.531
    • Rezzolla, L.1    Lamb, F.K.2    Shapiro, S.L.3
  • 15
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    • to be published
    • H. Spruit, Astron. Astrophys. 341, L1 (1999); L. Rezzolla, F. K. Lamb, and S. L. Shapiro, Astrophys. J. 531, L139 (2000); Y. Levin and G. Ushomirsky, Mon. Not. R. Astron. Soc. (to be published); W. C. G. Ho and D. Lai, Astrophys. J. (to be published).
    • Mon. Not. R. Astron. Soc.
    • Levin, Y.1    Ushomirsky, G.2
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    • to be published
    • H. Spruit, Astron. Astrophys. 341, L1 (1999); L. Rezzolla, F. K. Lamb, and S. L. Shapiro, Astrophys. J. 531, L139 (2000); Y. Levin and G. Ushomirsky, Mon. Not. R. Astron. Soc. (to be published); W. C. G. Ho and D. Lai, Astrophys. J. (to be published).
    • Astrophys. J.
    • Ho, W.C.G.1    Lai, D.2
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    • note
    • The difference between the actual and the predicted evolution of E (at early times) and J was due primarily to numerical error introduced by the Coriolis term in the rotating-frame evolution equations. A higher-order expression for this term has now been implemented, and even better agreement is expected in future simulations.
  • 19
    • 84889152195 scopus 로고    scopus 로고
    • note
    • In the barotropic hydrodynamic code used in this simulation, the structure of a shock is correctly evolved, but the energy dissipated in the shock is simply ignored.
  • 20
    • 84889134230 scopus 로고    scopus 로고
    • note
    • max decreases by 0.36% when κ is increased by the factor 4/3.


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