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DOE OSTI · 3021497

Magnetic flux emergence in binary neutron star remnants

Fields, Jacob [The Pennsylvania State University, University Park, PA (United States)] (ORCID:0000000157051712)·Radice, David [The Pennsylvania State University, University Park, PA (United States)] (ORCID:0000000169821008)·Hammond, Peter [The Pennsylvania State University, University Park, PA (United States); University of New Hampshire, Durham, NH (United States)] (ORCID:0000000294471043)
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Abstract

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 G, and more typical fields around 10 16 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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79 ASTRONOMY AND ASTROPHYSICSAstrophysical & cosmological simulationsAstrophysical electromagnetic fieldsAstrophysical fluid dynamicsBuoyancyDirect numerical simulationsFluids & classical fields in curved spacetimeGeneral relativityLagrangian flow fieldMagnetohydrodynamicsNeutron stars & pulsarsNumerical relativity

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Fields, Jacob [The Pennsylvania State University, University Park, PA (United States)] (ORCID:0000000157051712), Radice, David [The Pennsylvania State University, University Park, PA (United States)] (ORCID:0000000169821008), Hammond, Peter [The Pennsylvania State University, University Park, PA (United States); University of New Hampshire, Durham, NH (United States)] (ORCID:0000000294471043). 2026-02-25. Magnetic flux emergence in binary neutron star remnants. https://doi.org/10.1103/sqjg-l87v

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