TeV Pulsar Wind Nebulae in the CTA era
Abstract
The pulsar wind, a magnetized relativistic electron-positron plasma flow supplied from a pulsar, forms a shock as a result of the interaction with the surrounding supernova ejecta. The shocked pulsar wind is called pulsar wind nebula (PWN) which shines from radio through TeV gamma-rays via synchrotron radiation and inverse Compton scattering. The PWNe are an interesting laboratory for the investigations of the relativistic plasma dynamics such as particle acceleration, magnetic reconnection, the turbulence, and particle diffusion. Imaging atmospheric Cherenkov telescopes (H.E.S.S., MAGIC, and VERITAS) and also air shower arrays (MILAGRO, ARGO and HAWC) have detected dozens of TeV PWNe in our galaxy. Although almost half of the TeV sources in the galactic plane are not firmly identified in other wavelengths (TeV unID sources), PWNe are considered as a primary galactic TeV source. Most of the TeV unID sources would be old PWNe. Here, we will review the recent studies of broadband emission from PWNe and discuss the prospect for the CTA era focusing both on young and old PWNe.
- Publication:
-
43rd COSPAR Scientific Assembly. Held 28 January - 4 February
- Pub Date:
- January 2021
- Bibcode:
- 2021cosp...43E1286T