Speaker
Description
Magnetic fields and the associated turbulent dynamics are central to the evolution of binary neutron star merger remnants. In particular, the amplification of magnetic fields from realistic pre-merger seed strengths to the values thought to be required for jet launching, as well as the emergence of large-scale structures sustaining collimated relativistic outflows, remain not well understood. Addressing these questions is challenging because of both the complexity of relativistic MHD turbulence and the computational cost of fully nonlinear direct numerical relativity simulations.
In this talk, I will discuss recent simulations aimed at clarifying the role of the post-merger magnetic field configuration in setting the conditions for jet launching. I will compare simulations initialised with either a strong large-scale magnetic field or with a post-merger magnetic field calibrated to reproduce the magnetic spectrum obtained in previous large-eddy simulations. I will discuss how these different initial configurations affect the subsequent evolution of the remnant and examine their impact on diagnostics associated with the launching of relativistic jets.