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ROTATING NEUTRON STAR MODELS WITH MAGNETIC FIELD

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arxiv gr-qc/9503044 v1 pith:23DADKJT submitted 1995-03-25 gr-qc astro-ph

M. Bocquet , S. Bonazzola , E. Gourgoulhon , J. Novak This is my paper · ORCID
classification gr-qcastro-ph
keywords fieldmagneticmaximumneutronstarstarsmasseffects
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We present the first numerical solutions of the coupled Einstein-Maxwell equations describing rapidly rotating neutron stars endowed with a magnetic field. These solutions are fully relativistic and self-consistent, all the effects of the electromagnetic field on the star's equilibrium (Lorentz force, spacetime curvature generated by the electromagnetic stress-energy) being taken into account. The magnetic field is axisymmetric and poloidal. Five dense matter equations of state are employed. The partial differential equation system is integrated by means of a pseudo-spectral method. Various tests passed by the numerical code are presented. The effects of the magnetic field on neutron stars structure are then investigated, especially by comparing magnetized and non-magnetized configurations with the same baryon number. The deformation of the star induced by the magnetic field is important only for huge values of B (B>10^{10} T). The maximum mass as well as the maximum rotational velocity are found to increase with the magnetic field. The maximum allowable poloidal magnetic field is of the order of 10^{14} T (10^{18} G) and is reached when the magnetic pressure is comparable to the fluid pressure at the centre of the star. For such values, the maximum mass of neutron stars is found to increase by 13 to 29 % (depending upon the EOS) with respect to the maximum mass of non-magnetized stars.

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Cited by 9 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. OpenAlex reports about 40 citations worldwide. Full citation record

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    astro-ph.HE 2024-09 unverdicted novelty 8.0 of 10

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    A density-dependent bag EOS with Landau quantization produces strange quark stars up to 2.8 solar masses and deformation 1.55 at 1200 Hz and 5×10^17 G.

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  4. Electric, thermal and thermoelectric response of a hot pion gas in a time dependent background magnetic field

    hep-ph 2025-07 conditional novelty 6.0 of 10

    The transport coefficients of a hot pion gas are recalculated under exponentially decaying background magnetic fields, showing that the field lifetime changes conductivities, thermal conductivity, and Seebeck and Nern...

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  7. 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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  9. Spin effects in superfluidity, neutron matter and neutron stars

    astro-ph.HE 2026-04 unverdicted novelty 2.0 of 10

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