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Lindblom L, Tohline JE, Vallisneri M. Nonlinear evolution of the r-modes in neutron stars. Phys Rev Lett. 2001;86(7):1152-5doi: 10.1103/PhysRevLett.86.1152.
Lindblom, L., Tohline, J. E., & Vallisneri, M. (2001). Nonlinear evolution of the r-modes in neutron stars. Physical review letters, 86(7), 1152-5. https://doi.org/10.1103/PhysRevLett.86.1152
Lindblom, L, et al. "Nonlinear evolution of the r-modes in neutron stars." Physical review letters vol. 86,7 (2001): 1152-5. doi: https://doi.org/10.1103/PhysRevLett.86.1152
Lindblom L, Tohline JE, Vallisneri M. Nonlinear evolution of the r-modes in neutron stars. Phys Rev Lett. 2001 Feb 12;86(7):1152-5. doi: 10.1103/PhysRevLett.86.1152. PMID: 11178032.
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Phys Rev Lett. 2001 Feb 12;86(7):1152-5. doi: 10.1103/PhysRevLett.86.1152.

Nonlinear evolution of the r-modes in neutron stars.

Physical review letters

L Lindblom, J E Tohline, M Vallisneri

Affiliations

  1. Theoretical Astrophysics 130-33, California Institute of Technology, Pasadena, California 91125, USA.

PMID: 11178032 DOI: 10.1103/PhysRevLett.86.1152

Abstract

The evolution of a neutron-star r-mode driven unstable by gravitational radiation is studied here using numerical solutions of the full nonlinear fluid equations. The dimensionless amplitude of the mode grows to order unity before strong shocks develop which quickly damp the mode. In this simulation the star loses about 40% of its initial angular momentum and 50% of its rotational kinetic energy before the mode is damped. The nonlinear evolution causes the fluid to develop strong differential rotation which is concentrated near the surface and poles of the star.

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