Dynamical Rotational Instability at Low $T/W$

Joan M. Centrella; Kimberly C. B. New; Lisa L. Lowe; J. David Brown

doi:10.1086/319634

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arXiv · astro-ph/0010574

Dynamical Rotational Instability at Low $T/W$

Joan M. Centrella·Kimberly C. B. New·Lisa L. Lowe·J. David Brown

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Abstract

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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Joan M. Centrella, Kimberly C. B. New, Lisa L. Lowe, J. David Brown. 2000-10-27. Dynamical Rotational Instability at Low $T/W$. https://doi.org/10.1086/319634

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