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

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

2000-10-31

arxiv.org/abs/astro-ph/0010653v2

Phys.Rev.Lett. 86 (2001) 1152-1155

Astronomy and Astrophysics

Astrophysics

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

Scientific paper

10.1103/PhysRevLett.86.1152

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.

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