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Jet-environment interplay in magnetized binary neutron star mergers. (arXiv:2211.10135v2 [astro-ph.HE] UPDATED)

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GRB 170817A, the first short gamma-ray burst (sGRB) to be detected in
coincidence with a gravitational wave signal, demonstrated that merging binary
neutron star (BNS) systems can power collimated ultra-relativistic jets and, in
turn, produce sGRBs. Moreover, it revealed that sGRB jets possess an intrinsic
angular structure that is imprinted in the observable prompt and afterglow
emission. Advanced numerical simulations represent the leading approach to
investigate the physical processes underlying the evolution of sGRB jets
breaking out of post-merger environments, and thus connect the final angular
structure and energetics with specific jet launching conditions. In a previous
paper, we carried out the first three-dimensional (3D) special-relativistic
hydrodynamic simulations of incipient (top-hat) sGRB jets propagating across
the realistic environment resulting from a general-relativistic (GR)
hydrodynamic BNS merger simulation. While the above work marked an important
step toward a consistent end-to-end description of sGRB jets from BNS mergers,
those simulations did not account for the presence of magnetic fields, which
are expected to play a key role. Here, we overcome this limitation, reporting
the first 3D special-relativistic magnetohydrodynamic (MHD) simulation of a
magnetized (structured and rotating) sGRB jet piercing through a realistic
magnetized post-merger environment, wherein the initial conditions of the
latter are directly imported from the outcome of a previous GRMHD BNS merger
simulation.

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