Magnetosphere Evolution and Precursor-Driven Electromagnetic Signals in Merging Binary Neutron Stars

We detail new force-free simulations to investigate magnetosphere evolution and precursor electromagnetic (EM) signals from binary neutron stars. Our simulations fully follow a representative inspiral motion, capturing the intricate magnetospheric dynamics and their impact on EM outflows. We explore a range of stellar magnetic moment orientations and relative strengths, finding that the magnetospheres and Poynting flux evolution are strongly configuration-dependent. The Poynting flux exhibits pulsations at twice the orbital frequency, $2\Omega$, and is highly anisotropic, following a power-law dependence on orbital frequency. The index ranges from 1 to 6, shaped by the intricate dynamics of the magnetospheres. Furthermore, we present the first computation of: (1) The EM forces acting on the star surfaces, revealing the presence of torques that, for highly-magnetized stars, could influence the orbital dynamics or break the crust. (2) The high-energy emission signals from these systems by adopting the established isolated pulsar theory. Assuming curvature radiation in the radiation reaction limit, we find that photons could reach TeV--PeV energies in the last $\sim$~ms for magnetic field strengths $10^{10}-10^{15}$~G. However, our analysis of single photon magnetic pair production suggests that these photons are unlikely to escape, with the MeV band emerging as a promising observational window for precursor high-energy emission. In this framework, we construct high-energy emission skymaps and light curves, exploring observational implications. Finally, we propose potential precursor radio emission and delayed afterglow echoes from magnetized outflows, which may contribute to late-time re-brightening in short gamma-ray bursts or to orphan afterglows.