In quasi-topological gravity, neutron stars can surpass black-hole compactness with universal high-density behavior and theory corrections that stabilize radially unstable configurations from general relativity.
The w-mode instability of ultracompact relativistic stars
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abstract
In this article we show that the, mainly spacetime, w-modes may become unstable in a rotating ultracompact ($R<3M$) relativistic star. We provide results for the axial modes of a rotating star in the slow rotation approximation, and demonstrate that an instability may become active in stars with an ergosphere. These results suggest that the so-called ``ergoregion instability'' discussed by other authors is, in fact, associated with the w-modes of the star. The unstable modes are found to grow on a timescale of seconds to minutes. We discuss briefly whether the instability is likely to have any astrophysical relevance.
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gr-qc 1years
2026 1verdicts
UNVERDICTED 1representative citing papers
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Neutron stars more compact than black holes in quasi-topological gravity: Equilibrium configurations and radial stability
In quasi-topological gravity, neutron stars can surpass black-hole compactness with universal high-density behavior and theory corrections that stabilize radially unstable configurations from general relativity.