Rotational Instabilities and Centrifugal Hangup

Details Rotational Instabilities and Centrifugal Hangup Rotational Instabilities and Centrifugal Hangup

2001-01-17

arxiv.org/abs/gr-qc/0101071v1

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

13 pages (includes 11 figures) and 1 separate jpeg figure; to appear in Astrophysical Sources of Gravitational Radiation, AIP

Scientific paper

10.1063/1.1387314

One interesting class of gravitational radiation sources includes rapidly rotating astrophysical objects that encounter dynamical instabilities. We have carried out a set of simulations of rotationally induced instabilities in differentially rotating polytropes. An $n$=1.5 polytrope with the Maclaurin rotation law will encounter the $m$=2 bar instability at $T/|W| \gtrsim 0.27$. Our results indicate that the remnant of this instability is a persistent bar-like structure that emits a long-lived gravitational radiation signal. Furthermore, dynamical instability is shown to occur in $n$=3.33 polytropes with the $j$-constant rotation law at $T/|W| \gtrsim 0.14$. In this case, the dominant mode of instability is $m$=1. Such instability may allow a centrifugally-hung core to begin collapsing to neutron star densities on a dynamical timescale. If it occurs in a supermassive star, it may produce gravitational radiation detectable by LISA.

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