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Gravitational Radiation Instability in Hot Young Neutron Stars

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arxiv gr-qc/9803053 v1 pith:VXD3G7JE submitted 1998-03-13 gr-qc

Lee Lindblom , Benjamin J. Owen , Sharon M. Morsink This is my paper · ORCID
classification gr-qc
keywords instabilityneutronstarsangulargravitationalradiationrapidlyrotating
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We show that gravitational radiation drives an instability in hot young rapidly rotating neutron stars. This instability occurs primarily in the l=2 r-mode and will carry away most of the angular momentum of a rapidly rotating star by gravitational radiation. On the timescale needed to cool a young neutron star to about T=10^9 K (about one year) this instability can reduce the rotation rate of a rapidly rotating star to about 0.076\Omega_K, where \Omega_K is the Keplerian angular velocity where mass shedding occurs. In older colder neutron stars this instability is suppressed by viscous effects, allowing older stars to be spun up by accretion to larger angular velocities.

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Cited by 6 Pith papers

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    Using causal BDNK hydrodynamics, the authors derive coupled gravitational-wave and viscous-mode equations for slowly rotating stars and find superradiant amplification at low frequencies.

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  3. Particle Probes with Superradiant Pulsars

    hep-ph 2019-08 conditional novelty 6.0 of 10

    The existence of PSR J1748-2446ad and PSR B1937+21 excludes ultralight scalars coupled to neutrons with masses near 10^-11 eV at couplings as small as 10^-6 times gravity.

  4. PSR J0952-0607: Probing the Stiffest Equations of State and r-Mode Suppression Mechanisms

    astro-ph.HE 2025-02 conditional novelty 5.0 of 10

    Using the 709.2 Hz spin of PSR J0952-0607 in Bayesian equation-of-state inference shifts its inferred non-rotating mass to 2.10+0.25-0.24 Msun and makes r-mode stability depend on crust rigidity.

  5. Modelling Dissipative Dynamics of r-mode Instability in Hybrid Stars

    astro-ph.HE 2026-06 unverdicted novelty 4.0 of 10

    Bayesian inference on observational data yields shear viscosity timescale τ_s=(4.99^{+0.49}_{-0.52})×10^8 T^{5/3} s and bulk viscosity timescale for two-layer hybrid stars, giving frequency minima of 451.87 Hz and 517...

  6. Phase transitions in neutron stars and their links to gravitational waves

    astro-ph.HE 2019-07 unverdicted novelty 2.0 of 10

    Review of neutron star dense matter, hadron-quark phase transitions, and potential g-mode signatures in gravitational waves from multimessenger observations.

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