Dynamical Rotational Instability at Low $T/W$

Details Dynamical Rotational Instability at Low $T/W$ Dynamical Rotational Instability at Low $T/W$

2000-10-27

arxiv.org/abs/astro-ph/0010574v1

Astrophys.J. 550 (2001) L193-L196

Astronomy and Astrophysics

Astrophysics

5 pages, 4 figures; submitted to The Astrophysical Journal Letters

Scientific paper

10.1086/319634

Dynamical instability is shown to occur in differentially rotating polytropes with N = 3.33 and $T/|W| \gtrsim 0.14$. This instability has a strong m=1 mode, although the m=2, 3, and 4 modes also appear. Such instability may allow a centrifugally-hung core to begin collapsing to neutron star densities on a dynamical timescale. The gravitational radiation emitted by such unstable cores may be detectable with advanced ground-based detectors, such as LIGO II. If the instability occurs in a supermassive star, it may produce gravitational radiation detectable by the space-based detector LISA.

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