Speaker
Description
Accretion disks and astrophysical jets are typically found in several sources, e.g., young stellar objects, X-ray binaries, gamma-ray bursts, or active galactic nuclei. The origin and impact of a large-scale magnetic field on the dynamical and radiative features of disks and jets is still unclear. First, I will briefly discuss dynamo processes within thin accretion disks, able to amplify the magnetic field up to the point where jet launching becomes possible, focusing on how to build a more consistent dynamo and diffusivity model. Then I will present the first numerical simulations of resistive relativistic jets and the role of magnetic reconnection and dissipation in the large-scale simulations, focusing on short gamma-ray-burst jets. Such simulations investigate different values and models for the plasma resistivity coefficient, assessing their impact on the level of turbulence, the formation of current sheets and reconnection plasmoids, and the electromagnetic energy content.
