Magnetic Reconnection on Jet-Accretion disk Systems

TL;DR

This paper discusses how fast magnetic reconnection, especially when driven by turbulence, plays a crucial role in accelerating particles and producing high-energy emissions in astrophysical systems like black holes and jets.

Contribution

It provides a review of the theory of turbulent fast magnetic reconnection and presents recent analytical and numerical studies demonstrating its significance in astrophysical particle acceleration.

Findings

Fast magnetic reconnection can efficiently accelerate particles to relativistic speeds.

Turbulence enhances the rate of magnetic reconnection in astrophysical environments.

Reconnection processes can explain high-energy non-thermal emissions in jets and black hole surroundings.

Abstract

Fast Magnetic Reconnection is currently regarded as an important process also beyond the solar system, specially in magnetically dominated regions of galactic and extragalactic sources like the surrounds of black holes and relativistic jets. In this lecture we discuss briefly the theory of fast magnetic reconnection, specially when driven by turbulence which is very frequent in Astrophysical flows, and its implications for relativistic particle acceleration. Then we discuss these processes in the context of the sources above, showing recent analytical and multidimensional numerical MHD studies that indicate that fast reconnection can be a powerful process to accelerate particles to relativistic velocities, produce the associated high energy non-thermal emission, and account for efficient conversion of magnetic into kinetic energy in these flows.