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

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.

arXiv comment7 pages, to appear in PRD rapid communication

References in corpus (38)

• The Proto-Magnetar Model for Gamma-Ray Bursts
• A fossil origin for the magnetic fields of A-stars and white dwarfs
• Stable magnetic fields in stellar interiors
• Axisymmetric magnetic fields in stars: relative strengths of poloidal and toroidal components
• Equilibrium models of relativistic stars with a toroidal magnetic field
• WhiskyMHD: a new numerical code for general relativistic magnetohydrodynamics
• Evolution of magnetized, differentially rotating neutron stars: Simulations in full general relativity
• A constrained scheme for Einstein equations based on Dirac gauge and spherical coordinates
• Twisted-torus configurations with large toroidal magnetic fields in relativistic stars
• Structure and deformations of strongly magnetized neutron stars with twisted torus configurations
• Relativistic stars with poloidal and toroidal magnetic fields and meridional flow
• Axisymmetric equilibrium models for magnetized neutron stars in General Relativity under the Conformally Flat Condition
• Relativistic models of magnetars: the twisted-torus magnetic field configuration
• Magnetohydrodynamics in full general relativity: Formulation and tests
• On the Stability of Non Force-Free Magnetic Equilibria in Stars
• Relativistic MHD in dynamical spacetimes: Improved EM gauge condition for AMR grids
• The stability of toroidal fields in stars
• Deriving formulations for numerical computation of binary neutron stars in quasicircular orbits
• Relativistic stars with purely toroidal magnetic fields
• The stability of poloidal magnetic fields in rotating stars
• Afterglow of binary neutron star merger
• Three dimensional evolution of differentially rotating magnetized neutron stars
• Non-conformally flat initial data for binary compact objects
• Binary neutron stars: Equilibrium models beyond spatial conformal flatness
• Non-axisymmetric instabilities of neutron star with toroidal magnetic fields
• Evolutions of Magnetized and Rotating Neutron Stars
• A new code for equilibriums and quasiequilibrium initial data of compact objects
• Grad-Shafranov equation in noncircular stationary axisymmetric spacetimes
• Magnetohydrodynamics in stationary and axisymmetric spacetimes: a fully covariant approach
• Stably stratified magnetized stars in general relativity
• Three Dimensional Magneto Hydrodynamical Simulations of Gravitational Collapse of a 15Msun Star
• Quasi-equilibrium models for triaxially deformed rotating compact stars
• Coexistence of oppositely flowing multi-$\phi$-currents: Key to large toroidal magnetic fields within stars
• Thermodynamics of magnetized binary compact objects
• New code for equilibriums and quasiequilibrium initial data of compact objects. II. Convergence tests and comparisons of binary black hole initial data
• Stationary, Axisymmetric Neutron Stars with Meridional Circulation in General Relativity
• Non-axisymmetric oscillations of rapidly rotating relativistic stars by conformal flatness approximation
• Perfect magnetohydrodynamics as a field theory

Cited by in corpus (20)

• Magnetars: the physics behind observations
• Rotating Stars in Relativity
• General relativistic models for rotating magnetized neutron stars in conformally flat spacetime
• New code for equilibriums and quasiequilibrium initial data of compact objects. IV. Rotating relativistic stars with mixed poloidal and toroidal magnetic fields
• Limiting magnetic field for minimal deformation of a magnetised neutron star
• Magnetohydrodynamic simulations of self-consistent rotating neutron stars with mixed poloidal and toroidal magnetic fields
• Quasi-universality of the magnetic deformation of neutron stars in general relativity and beyond
• Conservation laws and evolution schemes in geodesic, hydrodynamic and magnetohydrodynamic flows
• Axisymmetric equilibrium models for magnetised neutron stars in Scalar-Tensor Theories
• Evolution of magnetic deformation in neutron star crust
• Stably stratified stars containing magnetic fields whose toroidal components are much larger than the poloidal ones in general relativity: A perturbation analysis
• 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
• Equilibriums of extremely magnetized compact stars with force-free magnetotunnels
• General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars
• Strong toroidal magnetic fields sustained by the elastic crust in a neutron star
• Methods for relativistic self-gravitating fluids: From binary neutron stars to black hole-disks and magnetized rotating neutron stars
• Interlinking internal and external magnetic fields of relativistically rotating neutron stars
• The Parallel Compact Object CALculator: An Efficient General Relativistic Initial Data Solver for Compact Objects
• Detectability of continuous gravitational waves from magnetically deformed neutron stars