Escape of High Energy Particles from Bow-Shock Pulsar Wind Nebulae
Date Issued
2018
Author(s)
Abstract
The detection of bright X-ray features and large TeV halos around old pulsars
that have escaped their parent Supernova Remnants and are interacting directly
with the ISM, suggest that high energy particles, more likely high energy
pairs, can escape from these systems, and that this escape if far more complex
than a simple diffusive model can predict. Here we present for the first time a
detailed analysis of how high energy particles escape from the head of the bow
shock. In particular we focus our attention on the role of the magnetic field
geometry, and the inclination of the pulsar spin axis with respect to the
direction of the pulsar kick velocity. We show that asymmetries in the escape
pattern of charged particles are common, and they are strongly energy
dependent. More interestingly we show that the flow of particles from bow-shock
pulsar wind nebulae is likely to be charge separated, which might have profound
consequences on the way such flow interacts with the ISM magnetic field,
driving local turbulence.
Volume
480
Issue
4
Start page
5419
Issn Identifier
0035-8711
Ads BibCode
2018MNRAS.480.5419B
Rights
open.access
File(s)![Thumbnail Image]()
![Thumbnail Image]()
Loading...
Name
28058-sty2237_P02.pdf
Description
Miur
Size
3.62 MB
Format
Adobe PDF
Checksum (MD5)
148f029d26a97eeae41b16ef34d7c995
Loading...
Name
sty2237.pdf
Description
Pdf editoriale
Size
11.3 MB
Format
Adobe PDF
Checksum (MD5)
e024591d246e3bfb2b75ef92974e1682