Orateur
Description
Turbulence plays a fundamental role in the transfer, amplification, and dissipation of magnetic and kinetic energy in astrophysical plasmas, from the solar corona to the vicinity of compact objects. In compact objects, including neutron stars, neutron star merger remnants and black-hole accretion flows, turbulent motions are crucial as they drive angular momentum transport, magnetic reconnection, particle acceleration, plasma heating and the generation of large-scale magnetic fields through dynamo action.
This talk will describe our current understanding of turbulence and dynamos in compact-object systems, with a particular emphasis on neutron stars in core-collapse supernova and neutron-star mergers and their remnants, but also on accretion disks around black holes. I will discuss how small-scale instabilities, such as convective instabilities, shear-driven turbulence the magneto-rotational instability, amplify magnetic fields and drive nonlinear turbulent cascades. I will show how these may lead to the generation of large-scale magnetic fields through mean-field dynamo processes and notably form the most magnetized neutron stars, magnetars. These large-scale magnetic fields can also launch relativistic jets in both core-collapse supernova and binary neutron star mergers. The goal of this talk is to provide a broad overview of how turbulence and dynamo action shape compact-object environments and to stimulate discussion on the common plasma processes that connect high-energy astrophysics and heliospheric science.