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Deformation of relativistic magnetized stars

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arxiv gr-qc/9910038 v1 pith:WZYIJLSS submitted 1999-10-12 gr-qc astro-ph

K. Konno , T. Obata , Y. Kojima This is my paper · ORCID
classification gr-qcastro-ph
keywords magneticenergyrelativisticstarsdeformationellipticitymodelsbecomes
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We formulate deformation of relativistic stars due to the magnetic stress, considering the magnetic fields to be perturbations from spherical stars. The ellipticity for the dipole magnetic field is calculated for some stellar models. We have found that the ellipticity becomes large with increase of a relativistic factor for the models with the same energy ratio of the magnetic energy to the gravitational energy.

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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. New Universal Relations for Magnetized Neutron Stars

    gr-qc 2026-08 conditional novelty 7.0 of 10

    Magnetized neutron stars with dipole fields obey a new exact relation between dipole moment and compactness, and approximate EoS-insensitive relations among dipole moment, quadrupole moment, and ellipticity.

  2. Shirokov and Shapiro Effects in the Hartle-Thorne Spacetime

    gr-qc 2026-05 unverdicted novelty 5.0 of 10

    In the Hartle-Thorne metric, angular momentum J and quadrupole moment Q couple radial and azimuthal oscillations in the Shirokov effect and alter Shapiro time delay, with oblate shapes increasing delay and frame-dragg...

  3. Magnetized neutron stars: perturbative versus fully-numerical approaches

    astro-ph.HE 2026-05 conditional novelty 4.0 of 10

    Direct comparison of Konno-99 perturbative and LORENE numerical methods for poloidal magnetized neutron stars shows perturbative validity for observed fields up to ~10^16 G and numerical resolution limits below ~10^10 G.

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