High-resolution GR neutrino-radiation MHD simulation of 1.35-1.35 Msun BNS merger shows KHI-driven B-field amplification to magnetar levels (~10^50 erg, factor >=316) in 3 ms post-merger.
Title resolution pending
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
citation-role summary
background 2
citation-polarity summary
fields
astro-ph.HE 3roles
background 2representative citing papers
3D GRMHD simulations with second-moment neutrino transport show aligned spins produce more collimated polar outflows and 2.4e-3 solar masses of proton-rich material yielding light r-process elements like 56Ni, while antialigned spins disrupt magnetic amplification.
Neutron dark decays modify the equation of state and either mildly suppress or strongly enhance bulk viscosity in neutron star merger conditions, depending on the in-medium decay rate.
citing papers explorer
-
A magnetar formation in binary neutron star merger
High-resolution GR neutrino-radiation MHD simulation of 1.35-1.35 Msun BNS merger shows KHI-driven B-field amplification to magnetar levels (~10^50 erg, factor >=316) in 3 ms post-merger.
-
Magnetic Eruption and Nucleosynthesis in GR{\nu}MHD Simulations of Spinning Neutron Star Mergers
3D GRMHD simulations with second-moment neutrino transport show aligned spins produce more collimated polar outflows and 2.4e-3 solar masses of proton-rich material yielding light r-process elements like 56Ni, while antialigned spins disrupt magnetic amplification.