Magnetic Reconnection on Jet-Accretion Disk Systems

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.

Magnetic reconnection, Cosmic Ray Acceleration and Gamma-Ray emission around Black Holes and Relativistic Jets

“…[70,53]), the evidences above led to a more detailed investigation of particle acceleration scenarios involving the production of the VHE in the coronal region of the accreting BH (see [41,46,44] and references therein). If such environments are magnetically dominated, as generally believed, then fast magnetic reconnection could be unavoidable, natural, and even efficient [18,16,21,75].…”

“…We will also argue about neutrino emission counterparts. Recent reviews on this subject can be also found in [16,21,17,75] to mention a few.…”

Harvesting energy driven by Comisso-Asenjo process from Kerr-MOG black holes

“…[104] or Gouveia Dal Pino and collaborators in refs. [105][106][107][108]. In the CAP, the reconnection zone is filled with flux ropes/plasmoids, which gives rise to fast magnetic reconnection while in [104] the reconnection zone is laminar, which gives rise to slow magnetic reconnection.…”

“…[105][106][107][108], the reconnection is in the collisional turbulent regime, which typically gives a fast reconnection regime. The differences in the reconnection zones lead to different inflow and outflow velocity formulas between [30,104], and [105][106][107][108]. The effectiveness of the magnetic reconnection process is therefore strongly regulated by these differences.…”

“…On the other hand, in the models discussed in refs. [105][106][107][108], the magnetic reconnection occurs between the corona of the accretion disk and the jet of the black hole, meaning that the X-point is located outside the ergosphere, and no energy can be extracted from the black hole. Now let us address analytically the plasma energy density which is essential for energy extraction.…”