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Turbulence modelling in neutron star merger simulations
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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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Cited by 2 Pith papers
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Transport Properties of the MRI in Differentially Rotating Neutron Stars
Saturated MRI turbulence in differentially rotating neutron stars yields ℓ_mix ≈ (0.01–0.1) λ_MRI, largely independent of density, so standard GRLES mixing-length prescriptions overestimate transport by about an order...
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SPH methods in the modelling of compact objects
An updated expert review of Newtonian and general-relativistic SPH for compact-object mergers, arguing that modern SPH variants with better kernels, steered dissipation and reproducing gradients match grid-based codes...
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