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 of magnitude.
General relativistic magnetohydrodynamics simulations for binary neutron star mergers
1 Pith paper cite this work. Polarity classification is still indexing.
1
Pith paper citing it
abstract
Binary neutron star mergers used to be the most promising candidate for gravitational waves for ground-based gravitational wave detectors, such as advanced LIGO and advanced VIRGO. This was proved by the detection of gravitational waves from a binary neutron star merger in 2017. Numerical modeling is pivotal in predicting and interpreting binary neutron star mergers. This chapter reviews the progress of fully general relativistic magnetized binary neutron star merger simulations. From 2008 to 2024, about forty numerical relativity simulations of magnetized binary neutron star mergers were conducted with a different level of sophistication. This chapter aims to comprehensively view the magnetohydrodynamics effect in binary neutron star mergers by reviewing all the related works.
fields
astro-ph.HE 1years
2026 1verdicts
CONDITIONAL 1representative citing papers
citing papers explorer
-
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 of magnitude.