Modeling PWNe and their magnetic fields
Abstract
Pulsar Wind Nebulae (PWNe) and bow shock PWNe, their aged counterparts, are fascinating systems. Indeed they show a large variety of emission properties, evidence for particles accelerated to extreme energies and puzzling signatures indicating efficient particles escape and diffusion from the nebulae. Due to the very complex physics involved, their modeling has been for years a real challenge. The complex physics of acceleration, transport and emission in these systems is strongly dependent on the magnetic field structure and evolution. In the last few years, the availability of 3D models has allowed us to investigate the properties of the plasma flow and magnetic fields in PWNe, leading to a big step forward in the solution of some of the puzzles, like for instance the long standing ``sigma-problem'' highlighted from the modeling of the non-thermal emission of the Crab Nebula and other young PWNe. In recent works, also the signatures of the magnetic field geometry on the overall morphology of bow shock PWNe have been investigated, with a particular focus on X-ray emission properties and particle escape mechanisms. All the above aspects will be discussed in this talk by reviewing the latest results from 3D models of PWNe.
- Publication:
-
Supernova Remnants: An Odyssey in Space after Stellar Death II
- Pub Date:
- June 2019
- Bibcode:
- 2019sros.confE.187O