Using high-resolution athenak simulations of a twisted toroidal flux tube, we study the flux emergence of magnetic structures in the shear layer of a hot massive neutron star typical of a binary neutron star remnant. High-resolution simulations demonstrate that magnetic buoyant instabilities allow for emergence only for extremely large magnetic fields significantly exceeding ${10}^{17}\mathrm{G}$, and more typical fields around ${10}^{16}\mathrm{G}$ are instead dominated by hydrodynamic effects. Because merger remnants tend to be stable against hydrodynamic convection, our work places strong limitations on the mechanisms by which massive binary neutron star remnants can produce the magnetically-driven outflows needed to power jets.

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• Astrophysical fluid dynamics
• Fluids & classical fields in curved spacetime
• General relativity
• Magnetohydrodynamics
• Neutron stars & pulsars
• Astrophysical electromagnetic fields
• Buoyancy
• Astrophysical & cosmological simulations
• Direct numerical simulations
• Lagrangian flow field
• Numerical relativity