Equilibrium solutions of relativistic rotating stars with mixed poloidal and toroidal magnetic fields
arXiv:1410.3913 · doi:10.1103/PhysRevD.90.101501
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.
7 pages, to appear in PRD rapid communication
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Cited by in corpus (8)
- General relativistic models for rotating magnetized neutron stars in conformally flat spacetime
- Limiting magnetic field for minimal deformation of a magnetised neutron star
- Quasi-universality of the magnetic deformation of neutron stars in general relativity and beyond
- Axisymmetric equilibrium models for magnetised neutron stars in Scalar-Tensor Theories
- Evolution of magnetic deformation in neutron star crust
- Crust-core transition of a neutron star: effect of the temperature under strong magnetic fields
- Appearance of the prolate and the toroidal magnetic field dominated stars - Analytic approach
- Detectability of continuous gravitational waves from magnetically deformed neutron stars