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Modeling differential rotations of compact stars in equilibriums

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arxiv 1709.02643 v2 pith:3IIIJOLN submitted 2017-09-08 astro-ph.HE gr-qc

Koji Uryu , Antonios Tsokaros , Luca Baiotti , Filippo Galeazzi , Keisuke Taniguchi , Shin'ichirou Yoshida This is my paper · ORCID
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keywords starsrotatingcompactdifferentialrotationsdifferentiallyequilibriumsmasses
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Outcomes of numerical relativity simulations of massive core collapses or binary neutron star mergers with moderate masses suggest formations of rapidly and differentially rotating neutron stars. Subsequent fall back accretion may also amplify the degree of differential rotations. We propose new formulations for modeling differential rotations of those compact stars, and present selected solutions of differentially rotating, stationary, and axisymmetric compact stars in equilibriums. For the cases when rotating stars reach break-up velocities, the maximum masses of such rotating models are obtained.

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Cited by 3 Pith papers

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

  1. Magnetic effects on fundamental modes in rotating neutron stars with a purely toroidal magnetic field

    astro-ph.HE 2025-09 conditional novelty 6.0 of 10

    Even with both rotation and a toroidal magnetic field, neutron star fundamental-mode frequencies stay quasi-linear in compactness and T/|W|, with magnetization-dependent slopes, and the f_2f/f_F ratio can help constra...

  2. Axisymmetric stability of neutron stars as extreme rotators in massive scalar-tensor theory

    gr-qc 2025-02 conditional novelty 6.0 of 10

    Differentially rotating scalarized neutron stars with enormous angular momentum are axisymmetrically stable up to the turning point of their mass sequence, beyond which they collapse to black holes, confirming the tur...

  3. Hybrid Stars with Post-Merger Rotation Profiles

    gr-qc 2026-06 unverdicted novelty 5.0 of 10

    Differential rotation in hybrid stars with deconfinement phase transition allows quasi-toroidal configurations with quark matter rings and leads to degeneracies in rotational profiles at mass-radius curve intersections.

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