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Long-term neutrino-radiation resistive-magnetohydrodynamics simulations infull general relativity are performed for a system composed of a massiveneutron star and a torus formed as a remnant of binary neutron star mergers.The simulation is performed in axial symmetry incorporating a mean-field dynamoterm for a hypothetical amplification of the magnetic-field strength. We firstcalibrate the mean-field dynamo parameters by comparing the results for theevolution of black hole-disk systems with viscous hydrodynamics results. Wethen perform simulations for the system of a remnant massive neutron star and atorus. As in the viscous hydrodynamics case, the mass ejection occurs primarilyfrom the torus surrounding the massive neutron star. The total ejecta mass andelectron fraction in the new simulation are similar to those in the viscoushydrodynamics case. However, the velocity of the ejecta can be significantlyenhanced by magnetohydrodynamics effects caused by global magnetic fields.

Long-term evolution of neutron-star merger remnants in general relativistic resistive-magnetohydrodynamics with a mean-field dynamo term