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-toroidal energy ratio over 100 ms.
ROTATING NEUTRON STAR MODELS WITH MAGNETIC FIELD
6 Pith papers cite this work. Polarity classification is still indexing.
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abstract
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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Rigidly rotating charged perfect fluids with constant density or polytropic equations of state can be immersed in the Wald magnetosphere while satisfying integrated conservation laws that reduce to modified Einstein-Euler equations.
In the NJL model, increasing isospin chemical potential favors pion superfluidity at small magnetic fields and rho superconductivity at large magnetic fields.
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.
Strong magnetic fields in compact stars induce Landau quantization and magnetic-moment couplings that change the equation of state and allow additional degrees of freedom such as hyperons, Delta resonances, and quark matter.
A review of spin effects, superfluidity, and magnetic fields in neutron matter and their influence on neutron-star structure, superfluid phases, and rotational dynamics.
citing papers explorer
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General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars
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-toroidal energy ratio over 100 ms.
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Relativistic figures of equilibrium in the Wald magnetosphere
Rigidly rotating charged perfect fluids with constant density or polytropic equations of state can be immersed in the Wald magnetosphere while satisfying integrated conservation laws that reduce to modified Einstein-Euler equations.
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QCD phase transition at finite isospin density and magnetic field
In the NJL model, increasing isospin chemical potential favors pion superfluidity at small magnetic fields and rho superconductivity at large magnetic fields.
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Magnetized neutron stars: perturbative versus fully-numerical approaches
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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Dense Matter and Compact Stars in Strong Magnetic Fields
Strong magnetic fields in compact stars induce Landau quantization and magnetic-moment couplings that change the equation of state and allow additional degrees of freedom such as hyperons, Delta resonances, and quark matter.
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Spin effects in superfluidity, neutron matter and neutron stars
A review of spin effects, superfluidity, and magnetic fields in neutron matter and their influence on neutron-star structure, superfluid phases, and rotational dynamics.