Nonlinear Evolution of the r-Modes in Neutron Stars

Lee Lindblom, Joel E. Tohline, and Michele Vallisneri
Phys. Rev. Lett. 86, 1152 – Published 12 February 2001
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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.

  • Received 31 October 2000

DOI:https://doi.org/10.1103/PhysRevLett.86.1152

©2001 American Physical Society

Authors & Affiliations

Lee Lindblom1, Joel E. Tohline2, and Michele Vallisneri1,3

  • 1Theoretical Astrophysics 130-33, California Institute of Technology, Pasadena, California 91125
  • 2Department of Physics and Astronomy, Louisiana State University, Baton Rouge, Louisiana 70803
  • 3INFN, Sezione di Milano, Gruppo Collegato di Parma/Università di Parma, 43100 Parma, Italy

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Issue

Vol. 86, Iss. 7 — 12 February 2001

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