Impact of a mean field dynamo on neutron star mergers leading to magnetar remnants

Most, Elias R.

doi:10.1103/physrevd.108.123012

Phys. Rev. D

2023

DOI: 10.1103/physrevd.108.123012

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Impact of a mean field dynamo on neutron star mergers leading to magnetar remnants

Elias R. Most

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2024

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Cited by 5 publications

References 127 publications

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Turbulence modelling in neutron star merger simulations

Radice,

Hawke

2024

Living Rev Comput Astrophys

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Observations of neutron star mergers have the potential to unveil detailed physics of matter and gravity in regimes inaccessible by other experiments. Quantitative comparisons to theory and parameter estimation require nonlinear numerical simulations. However, the detailed physics of energy and momentum transfer between different scales, and the formation and interaction of small scale structures, which can be probed by detectors, are not captured by current simulations. This is where turbulence enters neutron star modelling. This review will outline the theory and current status of turbulence modelling for relativistic neutron star merger simulations.

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Turbulence modelling in neutron star merger simulations

Radice,

Hawke

2024

Living Rev Comput Astrophys

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Anisotropic energy injection from magnetar central engines in short GRBs

Wang,

Zhang,

Zhu

2024

Monthly Notices of the Royal Astronomical Society

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A long-lived magnetar, potentially originating from a binary neutron star system, has been proposed to explain the extended emission observed in certain short-duration gamma-ray bursts (sGRBs), and is posited as a potential central engine to power the engine-fed kilonovae. Previously, the process by which energy is injected into the surrounding ejecta/jet was widely believed to be nearly isotropic. In this study, we employ special relativity magnetohydrodynamic (SRMHD) simulations to investigate the wind injection process from a magnetar central engine. We explore the dynamics and energy distribution within the system and found that the parameter α = uA/uMWN can be used to indicate the collimation of the magnetar wind energy injection, where uA is the local Alfven four-speed and uMWN is the four-speed of the magnetar wind nebular (MWN) formed from wind-ejecta collision. A significant portion of the injected energy from the magnetar spin-down wind will be channeled to the jet axis due to collimation within the MWN. Achieving isotropic energy injection requires a significantly small α that necessitates either an ultra-relativistic expanding MWN or an extremely low magnetization MWN, both of which are challenging to attain in sGRBs. Consequently, a considerably reduced energy budget (i.e. energy per solid angle reduced by a factor of up to 10 with respect to the value under isotropic assumption) is anticipated to be injected into the ejecta for engine-fed kilonovae. Engine-fed kilonovae would appear fainter than originally anticipated.

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General-relativistic gauge-invariant magnetic helicity transport: Basic formulation and application to neutron star mergers

Wu,

Most

2024

Phys. Rev. D

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Impact of a mean field dynamo on neutron star mergers leading to magnetar remnants

Cited by 5 publications

References 127 publications

Turbulence modelling in neutron star merger simulations

Turbulence modelling in neutron star merger simulations

Anisotropic energy injection from magnetar central engines in short GRBs

General-relativistic gauge-invariant magnetic helicity transport: Basic formulation and application to neutron star mergers

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