Dynamical Rotational Instability at Low T/W
Joan M. Centrella, Kimberly C. B. New, Lisa L. Lowe, J. David Brown
Abstract
Dynamical instability is shown to occur in differentially rotating polytropes with N = 3.33 and T/|W| 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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