Non-Linear Evolution of the r-Modes in Neutron Stars

Abstract

The evolution of a neutron-star r-mode driven unstable by gravitational radiation (GR) is studied here using numerical solutions of the full non-linear fluid equations. The 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 non-linear evolution causes the fluid to develop strong differential rotation which is concentrated near the surface and especially near the poles of the star.

4 pages, 7 eps figures, revtex; revised, typos corrected

References in corpus (1)

• Nonlinear r-modes in Rapidly Rotating Relativistic Stars

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