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B. J. Owen, L. Lindblom, C. Cutler, B. F. Schutz, A. Vecchio, and N. Andersson, Phys. Rev. D 58, 084020 (1998).
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Owen, B.J.1
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Cutler, C.3
Schutz, B.F.4
Vecchio, A.5
Andersson, N.6
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5
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4243909304
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preceding Letter
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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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Phys. Rev. Lett.
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Stergioulas, N.1
Font, J.A.2
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L. Rezzolla, M. Shibata, H. Asada, T. W. Baumgarte, and S. L. Shapiro, Astrophys. J. 525, 935 (1999).
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Astrophys. J.
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Rezzolla, L.1
Shibata, M.2
Asada, H.3
Baumgarte, T.W.4
Shapiro, S.L.5
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8
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21944443720
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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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Astrophys. J.
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New, K.C.B.1
Tohline, J.E.2
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9
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21944443720
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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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Astrophys. J.
, vol.527
, pp. 527
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Cohl, H.S.1
Tohline, J.E.2
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10
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0034164197
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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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Astrophys. J.
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Cazes, J.E.1
Tohline, J.E.2
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12
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84889104074
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note
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22.
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13
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0009793612
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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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(1999)
Astron. Astrophys.
, vol.341
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Spruit, H.1
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14
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0034628683
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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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(2000)
Astrophys. J.
, vol.531
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Rezzolla, L.1
Lamb, F.K.2
Shapiro, S.L.3
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15
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0009793612
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to be published
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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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Mon. Not. R. Astron. Soc.
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Levin, Y.1
Ushomirsky, G.2
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16
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0009793612
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to be published
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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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Astrophys. J.
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Ho, W.C.G.1
Lai, D.2
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18
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84889113786
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note
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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.
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19
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84889152195
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note
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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.
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20
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84889134230
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note
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max decreases by 0.36% when κ is increased by the factor 4/3.
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