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Comment on "Instabilities in Close Neutron Star Binaries"

Douglas M. Eardley·Eric W. Hirschmann
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Abstract

In a recent Physical Review Letter, Wilson and Mathews presented some interesting numerical calculations of a system of two equally massive neutron stars in strong-field gravity. In particular they estimated the innermost stable circular orbit in their system. Here we point out a possibly important consequence of their results: Their calculated configurations have total angular momentum $J$ and total mass $M$ too large to form any Kerr black hole: $J>M^2$, in constrast to previous calculations of the innermost stable circular orbit.

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Douglas M. Eardley, Eric W. Hirschmann. 1996-01-11. Comment on "Instabilities in Close Neutron Star Binaries". https://arxiv.org/abs/gr-qc/9601019

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