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Tidal deformability and radial oscillations of anisotropic polytropic spheres

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arxiv 2112.09729 v1 pith:K5FFEWH3 submitted 2021-12-17 gr-qc

José D. V. Arbañil , Grigoris Panotopoulos This is my paper · ORCID
classification gr-qc
keywords anisotropicdeformabilityradialtidalpolytropicequationoscillationsspheres
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abstract

We compute the equilibrium, the fundamental eigenfrequency of oscillations modes, and quadrupolar tidal deformability of anisotropic polytropic spheres. These studies are respectively performed through the numerical solution of the Tolman-Oppenheimer-Volkoff equation, Chandrasekhar radial oscillation equations, and nonlinear first-order Riccati equation for tidal deformability, all modified from their original version to include the anisotropic effects. For the polytropic exponent $\gamma=2$ and the anisotropic model of Cattoen, Faber, and Visser, we show that the anisotropy could be reflected in the radial pressure, energy density, speed of sound, radial stability, and tidal deformability.

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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. On Modeling Anisotropic Quark Stars: The Role of Anisotropy in Radial Oscillation Spectra

    gr-qc 2026-08 conditional novelty 6.0 of 10

    Radial oscillation spectra of an anisotropic strange quark star model of Cen X-3 are computed for three anisotropy prescriptions and differ by up to 40 percent between models.

  2. Examining the influence of anisotropy on the fundamental mode of nonradial oscillation in neutron stars on a complete general relativistic scheme

    gr-qc 2025-09 conditional novelty 6.0 of 10

    Pressure anisotropy in strange quark stars measurably changes the f-mode oscillation frequency and the dimensionless tidal deformability, with positive anisotropy increasing mass and deformability while lowering the f...

  3. Radial Oscillations of the HESS J1731-347 Compact Object via the Karmarkar Condition in Gravity

    gr-qc 2025-04 conditional novelty 5.0 of 10

    A Karmarkar-based anisotropic stellar model fits HESS J1731-347's mass and radius and predicts radial oscillation frequencies about 20-30% higher than the isotropic Tolman IV model.

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