Pith. sign in

REVIEW 3 cited by

New code for equilibriums and quasiequilibrium initial data of compact objects. IV. Rotating relativistic stars with mixed poloidal and toroidal magnetic fields

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 1906.10393 v1 pith:ZNKKV5R3 submitted 2019-06-25 gr-qc astro-ph.HE

New code for equilibriums and quasiequilibrium initial data of compact objects. IV. Rotating relativistic stars with mixed poloidal and toroidal magnetic fields

Koji Uryu , Shijun Yoshida , Eric Gourgoulhon , Charalampos Markakis , Kotaro Fujisawa , Antonios Tsokaros , Keisuke Taniguchi , Yoshiharu Eriguchi This is my paper
classification gr-qc astro-ph.HE
keywords compactmagnetizedtoroidalstarscodeequationsextremelyfields
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
0 comments
read the original abstract

A new code for computing fully general relativistic solutions of strongly magnetized rapidly rotating compact stars is developed as a part of the COCAL (Compact Object CALculator) code. The full set of Einstein's equations, Maxwell's equations and magnetohydrodynamic equations are consistently solved assuming perfect conductivity, stationarity, and axisymmetry, and strongly magnetized solutions associated with mixed poloidal and toroidal components of magnetic fields are successfully obtained in generic (non-circular) spacetimes. We introduce the formulation of the problem and the numerical method in detail, then present examples of extremely magnetized compact star solutions and their convergence tests. It is found that, in extremely magnetized stars, the stellar matter can be expelled from the region of strongest toroidal fields. Hence we conjecture that a toroidal electro-vacuum region may appear inside of the extremely magnetized compact stars, which may seem like the neutron star becoming the strongest toroidal solenoid coil in the universe.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 3 Pith papers

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

  1. General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars

    astro-ph.HE 2024-09 unverdicted novelty 8.0

    Resistive GRMHD simulations of rotating neutron stars show resistivity changes magnetic field geometries, suppresses instabilities, and lowers GW emission amplitude while maintaining a consistent 9:1 poloidal-to-toroi...

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

    astro-ph.HE 2026-05 conditional novelty 4.0

    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.

  3. Influence of neutrino-electron scattering and neutrino-pair annihilation on hypermassive neutron star

    astro-ph.HE 2024-10 unverdicted novelty 4.0

    Inelastic neutrino-electron scattering in hypermassive neutron star simulations increases disc mass by 75% and ejecta mass by 18% with higher neutrino luminosities, while electron-positron annihilation shows no signif...