Hostname: page-component-76fb5796d-2lccl Total loading time: 0 Render date: 2024-04-25T07:40:10.766Z Has data issue: false hasContentIssue false
  • English
  • Français

A shock model for quasars and active galactic nuclei*

Published online by Cambridge University Press:  19 July 2016

I. Pérez-Fournon  and
P. Biermann
I. Pérez-Fournon
Affiliation:
Instituto de Astrofísica de Canarias, 38071 La Laguna, Tenerife, Spain
P. Biermann
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 5300 Bonn 1, F. R. of Germany

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

First order Fermi acceleration is an efficient mechanism to produce relativistic particles in strong astrophysical shocks. We have developed a model using this theory to explain the non-thermal emission from non-relativistic jets in Quasars and AGNs. Fluid dynamical simulations of cosmic jets predict shock formation in them at quasi-periodic intervals. This is also suggested by observations of jets. We identify the shocks as the sites of reacceleration of the energetic particles required to explain the non-thermal emission of the jets. In order to facilitate the comparison with observations, we have done numerical simulations of the expected observational properties at high and low spatial resolution.

Type
IV. Prime Movers, Models and Mechanisms
Information
Symposium - International Astronomical Union , Volume 119: Quasars , 1986 , pp. 405 - 406
Copyright
Copyright © Reidel 1986 

References

Bregman, J.N.: 1985, Ap. J. 288, 32 Google Scholar
Marcaide, J.M. et al.: 1985, Astron. Astrophys. 142, 71 Google Scholar
Rieke, G.H., Lebofsky, M.J., Wiśniewski, W.Z.: 1982, Ap. J. 263, 73 CrossRefGoogle Scholar
Schlickeiser, R.: 1984, Astron. Astrophys. 136, 227 Google Scholar
Webb, G.M., Drury, L.O'C., Biermann, P.: 1984, Astron. Astrophys. 137, 185 Google Scholar