Equilibrium solutions of relativistic rotating stars with mixed poloidal and toroidal magnetic fields

Koji Uryu; Eric Gourgoulhon; Charalampos M. Markakis; Kotaro Fujisawa; Antonios Tsokaros; Yoshiharu Eriguchi

doi:10.1103/PhysRevD.90.101501

Equilibrium solutions of relativistic rotating stars with mixed poloidal and toroidal magnetic fields

Koji Uryu
, Eric Gourgoulhon
, Charalampos M. Markakis
, Kotaro Fujisawa
, Antonios Tsokaros
, Yoshiharu Eriguchi

Applied Mathematics and Statistics

University of the Ryukyus
Université PSL
Waseda University
Goethe University Frankfurt
Tokyo University of Science

Research output: Contribution to journal › Article › peer-review

30 Scopus citations

Abstract

Stationary and axisymmetric solutions of relativistic rotating stars with strong mixed poloidal and toroidal magnetic fields are obtained numerically. Because of the mixed components of the magnetic field, the underlying stationary and axisymmetric spacetimes are no longer circular. These configurations are computed from the full set of the Einstein-Maxwell equations, Maxwell's equations, and from first integrals and integrability conditions of the magnetohydrodynamic equilibrium equations. After a brief introduction of the formulation of the problem, we present the first results for highly deformed magnetized rotating compact stars.

Original language	English
Article number	101501
Journal	Physical Review D - Particles, Fields, Gravitation and Cosmology
Volume	90
Issue number	10
DOIs	https://doi.org/10.1103/PhysRevD.90.101501
State	Published - Nov 7 2014

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10.1103/PhysRevD.90.101501

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abstract = "Stationary and axisymmetric solutions of relativistic rotating stars with strong mixed poloidal and toroidal magnetic fields are obtained numerically. Because of the mixed components of the magnetic field, the underlying stationary and axisymmetric spacetimes are no longer circular. These configurations are computed from the full set of the Einstein-Maxwell equations, Maxwell's equations, and from first integrals and integrability conditions of the magnetohydrodynamic equilibrium equations. After a brief introduction of the formulation of the problem, we present the first results for highly deformed magnetized rotating compact stars.",

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AU - Uryu, Koji

AU - Gourgoulhon, Eric

AU - Markakis, Charalampos M.

AU - Fujisawa, Kotaro

AU - Tsokaros, Antonios

AU - Eriguchi, Yoshiharu

PY - 2014/11/7

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N2 - Stationary and axisymmetric solutions of relativistic rotating stars with strong mixed poloidal and toroidal magnetic fields are obtained numerically. Because of the mixed components of the magnetic field, the underlying stationary and axisymmetric spacetimes are no longer circular. These configurations are computed from the full set of the Einstein-Maxwell equations, Maxwell's equations, and from first integrals and integrability conditions of the magnetohydrodynamic equilibrium equations. After a brief introduction of the formulation of the problem, we present the first results for highly deformed magnetized rotating compact stars.

AB - Stationary and axisymmetric solutions of relativistic rotating stars with strong mixed poloidal and toroidal magnetic fields are obtained numerically. Because of the mixed components of the magnetic field, the underlying stationary and axisymmetric spacetimes are no longer circular. These configurations are computed from the full set of the Einstein-Maxwell equations, Maxwell's equations, and from first integrals and integrability conditions of the magnetohydrodynamic equilibrium equations. After a brief introduction of the formulation of the problem, we present the first results for highly deformed magnetized rotating compact stars.

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IS - 10

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ER -

Equilibrium solutions of relativistic rotating stars with mixed poloidal and toroidal magnetic fields

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