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.
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Shell-to-shell transfer analysis in decaying MHD turbulence demonstrates direct non-local inverse energy transfer from the integral scale, resulting in multiplicative growth of large-scale magnetic energy, confined within helical sectors when net helicity is zero.
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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.
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Inverse energy transfer in decaying MHD turbulence: A shell-to-shell analysis
Shell-to-shell transfer analysis in decaying MHD turbulence demonstrates direct non-local inverse energy transfer from the integral scale, resulting in multiplicative growth of large-scale magnetic energy, confined within helical sectors when net helicity is zero.