Numerical evolutions of nonlinear r-modes in neutron stars

Creators: Lindblom, Lee; Tohline, Joel E.; Vallisneri, Michele

Abstract

Nonlinear evolution of the gravitational radiation (GR) driven instability in the r-modes of neutron stars is studied by full numerical 3D hydrodynamical simulations. The growth of the r-mode instability is found to be limited by the formation of shocks and breaking waves when the dimensionless amplitude of the mode grows to about three in value. This maximum mode amplitude is shown by numerical tests to be rather insensitive to the strength of the GR driving force. Upper limits on the strengths of possible nonlinear mode-mode coupling are inferred. Previously unpublished details of the numerical techniques used are presented, and the results of numerous calibration runs are discussed.

Additional Information

© 2002 American Physical Society. (Received 20 September 2001; published 9 April 2002) We thank L. Bildsten, J. Friedman, Yu. Levin, B. Owen, N. Stergioulas, K. Thorne, G. Ushomirsky, and R. Wagoner for helpful discussions. We also thank H. Cohl, J. Cazes, and especially P. Motl for contributions to the LSU hydrodynamic code. This research was supported by NSF grants PHY-9796079, AST-9987344, AST-9731698, PHY-9900776, PHY-9907949, and PHY-0099568 and NASA grants NAG5-4093, NAG5-8497 and NAG5-10707. We thank NRAC for computing time on NPACI facilities at SDSC where tests were conducted; and we thank CACR for access to the HP V2500 computers at Caltech, where the primary simulations were performed.

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Published - PhysRevD.65.084039.pdf

Accepted Version - 0109352.pdf

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