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Limiting Rotation Rate of Neutron Stars from Crust Breaking and Gravitational Waves

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arxiv 2410.19111 v2 pith:JB3F44OA submitted 2024-10-24 astro-ph.HE gr-qcnucl-th

J. A. Morales , C. J. Horowitz This is my paper · ORCID
classification astro-ph.HEgr-qcnucl-th
keywords cruststarsgravitationalneutronratebreakupconfigurationellipticity
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Neutron stars are not observed to spin faster than about half their breakup rate. This limiting rotational frequency may be related to the strength of their crusts. As a star spins up from accretion, centrifugal forces stress the crust. We perform finite-element simulations of rotating neutron stars and find that the crust fails at rotation rates about half the breakup rate. Given uncertainties in microphysics, we have not determined the crust configuration after this failure. Instead, we argue that the crust may fail in an asymmetric way and could produce a configuration with a significant ellipticity (fractional difference in moments of inertia). If the ellipticity is large, a rotating star will radiate gravitational waves that may limit further spin up. These stars may be promising sources for LIGO / VIRGO and next generation gravitational wave detectors.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Assessing the Impact of Instrumental Requirements on the Scientific Performance of the Einstein Telescope

    astro-ph.IM 2026-07 accept novelty 6.0 of 10

    Degrading the Einstein Telescope's sensitivity in specific frequency bands hurts different science goals in predictable ways, but the mission remains scientifically strong even in the worst modelled cases.

  2. Constraining shear modulus of polycrystalline neutron star crust: Hashin-Shtrikman variational approach

    astro-ph.HE 2025-07 accept novelty 6.0 of 10

    Hashin-Shtrikman variational bounds show that the effective shear modulus of a polycrystalline neutron star crust is lower than the commonly assumed Voigt value, with narrower upper and lower limits.

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