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Fast Rotating Neutron Stars: Oscillations and Instabilities

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arxiv 2110.00393 v1 pith:YZKPIXMV submitted 2021-10-01 gr-qc

Christian J. Krüger , Kostas D. Kokkotas , Praveen Manoharan , Sebastian H. Völkel This is my paper · ORCID
classification gr-qc
keywords neutronoscillationsrotatingstarscompactfastnon-axisymmetricobjects
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In this review article, we present the main results from our most recent research concerning the oscillations of fast rotating neutron stars. We derive a set of time evolution equations for the investigation of non-axisymmetric oscillations of rapidly rotating compact objects in full general relativity, taking into account the contribution of a dynamic spacetime. Using our code, which features high accuracy at comparably low computational expense, we are able to extract the frequencies of non-axisymmetric modes of compact objects with rotation rates up to the Kepler limit. We propose various universal relations combining bulk properties of isolated neutron stars as well as of binary systems before and after merger; these relations are independent of the true equation of state and may serve as a valuable tool for gravitational wave asteroseismology. We also present an introductory example using a Bayesian analysis.

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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. The error budget of binary neutron star merger simulations for configurations with high spin

    gr-qc 2025-06 accept novelty 6.0 of 10

    For highly spinning (chi=0.5) binary neutron stars, evolution code choice is the largest numerical waveform error, and current analytical models disagree with numerical relativity beyond that error after the stars touch.

  2. Fastest spinning millisecond pulsars: indicators for quark matter in neutron stars?

    nucl-th 2024-12 conditional novelty 6.0 of 10

    Hybrid stars with color-superconducting quark matter can reproduce the mass and spin of pulsar J0952-0607, whereas the hadronic-only model cannot, and the revised Kepler-frequency relation tightens radius bounds.

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