Three-dimensional evolution of differentially rotating magnetized neutron stars

Kiuchi, Kenta; Kyutoku, Koutarou; Shibata, Masaru

doi:10.1103/physrevd.86.064008

Cited by 73 publications

(78 citation statements)

References 78 publications

(169 reference statements)

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“…Long-lived magnetars have been proposed to explain the prompt GRB emission or late-time X-ray activities of sGRBs based either on the spin-down luminosity (Fan & Xu 2006;Troja 2007;Metzger et al 2008;Rowlinson et al 2013;Gao et al 2015;Lü et al 2015;Siegel & Ciolfi 2016a, or on outflows powered by differential rotation (Shibata et al 2011;Kiuchi et al 2012;Siegel et al 2014). In fact, numerical simulations have recently shown strong amplification of magnetic fields at merger (Price & Rosswog 2006;Giacomazzo & Perna 2013;Giacomazzo et al 2015;Kiuchi et al 2015).…”

Section: Comparison With Previous Workmentioning

confidence: 99%

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Hotokezaka

Nissanke

Hallinan

et al. 2016

ApJ

113

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Mergers of binary neutron stars and black hole-neutron star binaries produce gravitational-wave(GW) emission and outflows with significant kinetic energies. These outflows result in radio emissions through synchrotron radiation. We explore the detectability of these synchrotron-generated radio signals by follow-up observations of GW merger events lacking a detection of electromagnetic counterparts in other wavelengths. We model radio light curves arising from (i) sub-relativistic merger ejecta and (ii) ultra-relativistic jets. The former produce radio remnants on timescales of a few years and the latter produce γ-ray bursts in the direction of the jet and orphan-radio afterglows extending over wider angles on timescales of weeks. Based on the derived light curves, we suggest an optimized survey at 1.4 GHz with five epochs separated by a logarithmic time interval. We estimate the detectability of the radio counterparts of simulated GW-merger events to be detected by advanced LIGO and Virgo by current and future radio facilities. The detectable distances for these GW merger events could be as high as 1 Gpc. Around 20%-60% of the long-lasting radio remnants will be detectable in the case of the moderate kinetic energy of 3 10 50 · erg and a circum-merger density of -0.1 cm 3 or larger, while 5%-20% of the orphan-radio afterglows with kinetic energy of 10 48 erg will be detectable. The detection likelihood increases if one focuses on the well-localizable GW events. We discuss the background noise due to radio fluxes of host galaxies and false positives arising from extragalactic radio transients and variable activegalacticnuclei, and we show that the quiet radio transient sky is of great advantage when searching for the radio counterparts.

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Section: Comparison With Previous Workmentioning

confidence: 99%

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Hotokezaka

Nissanke

Hallinan

et al. 2016

ApJ

113

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“…Constrained transport methods are often difficult to implement in simulations that employ mesh refinement, since maintaining balance at refinement boundaries is algorithmically complex. However, recently [97] have implemented a version of constrained transport that employs prolongation and restriction operators that preserve the divergence of the magnetic field. In this initial GRHydro MHD release we implement both divergence cleaning and constrained transport, both of which are detailed below.…”

Section: Divergence-free Constraint Treatmentmentioning

confidence: 99%

“…, (97) and the wavevector k = 2π/L x for one-dimensional cases. For two-dimensional cases, we rotate the coordinates so that wave fronts lie along diagonals of the grid.…”

Section: Alfvén Wavementioning

confidence: 99%

GRHydro: a new open-source general-relativistic magnetohydrodynamics code for the Einstein toolkit

Mösta

Mundim

Faber

et al. 2013

Class. Quantum Grav.

149

194

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We present the new general-relativistic magnetohydrodynamics (GRMHD) capabilities of the Einstein toolkit, an open-source community-driven numerical relativity and computational relativistic astrophysics code. The GRMHD extension of the toolkit builds upon previous releases and implements the evolution of relativistic magnetized fluids in the ideal MHD limit in fully dynamical spacetimes using the same shock-capturing techniques previously applied to hydrodynamical evolution. In order to maintain the divergence-free character of the magnetic field, the code implements both constrained transport and hyperbolic divergence cleaning schemes. We present test results for a number of MHD tests in Minkowski and curved spacetimes. Minkowski tests include aligned and oblique planar shocks, cylindrical explosions, magnetic rotors, Alfvén waves and advected loops, as well as a set of tests designed to study the response of the divergence cleaning scheme to numerically generated monopoles. We study the code's performance in curved spacetimes with spherical accretion onto a black hole on a fixed background spacetime and in fully dynamical spacetimes by evolutions of a magnetized polytropic neutron star and of the collapse of a magnetized stellar core. Our results agree well with exact solutions where these are available and we demonstrate convergence. All code and input files used to generate the results are available on http://einsteintoolkit.org. This makes our work fully reproducible and provides new users with an introduction to applications of the code.

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“…This scenario has recently been considered in Refs. [31,32], where numerical simulations of an axisymmetric differentially rotating HMNS were carried out. The HMNS had initially a purely poloidal magnetic field, which eventually led to a magnetically driven outflow along the rotation axis.…”

Section: Introductionmentioning

confidence: 99%

Dynamical bar-mode instability in rotating and magnetized relativistic stars

Franci¹,

Pietri²,

Dionysopoulou³

et al. 2013

Phys. Rev. D

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We present three-dimensional simulations of the dynamical bar-mode instability in magnetized and differentially rotating stars in full general relativity. Our focus is on the effects that magnetic fields have on the dynamics and the onset of the instability. In particular, we perform ideal-magnetohydrodynamics simulations of neutron stars that are known to be either stable or unstable against the purely hydrodynamical instability, but to which a poloidal magnetic field in the range of 10 14 -10 16 G is superimposed initially. As expected, the differential rotation is responsible for the shearing of the poloidal field and the consequent linear growth in time of the toroidal magnetic field. The latter rapidly exceeds in strength the original poloidal one, leading to a magnetic-field amplification in the the stars. Weak initial magnetic fields, i.e., 10 15 G, have negligible effects on the development of the dynamical bar-mode instability, simply braking the stellar configuration via magnetic-field shearing, and over a timescale for which we derived a simple algebraic expression. On the other hand, strong magnetic fields, i.e., 10 16 G, can suppress the instability completely, with the precise threshold being dependent also on the amount of rotation. As a result, it is unlikely that very highly magnetized neutron stars can be considered as sources of gravitational waves via the dynamical bar-mode instability.

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Three-dimensional evolution of differentially rotating magnetized neutron stars

Cited by 73 publications

References 78 publications

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

GRHydro: a new open-source general-relativistic magnetohydrodynamics code for the Einstein toolkit

Dynamical bar-mode instability in rotating and magnetized relativistic stars

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