Hostname: page-component-5c6d5d7d68-txr5j Total loading time: 0 Render date: 2024-08-25T03:17:10.292Z Has data issue: false hasContentIssue false
  • English
  • Français

Connections Between Turbulence and Jet Morphology

Published online by Cambridge University Press:  14 August 2015

Gregory Benford
Gregory Benford*
Affiliation:
Physics Department, University of California, Irvine Irvine, California 92717

Extract

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.

Radio jet morphologies may be caused by large-scale Kelvin-Helmholtz (KH) instabilities. If high-speed, pressure-confined fluid beams lie at the core of these jets, they are susceptible to KH modes, as studied by a number of authors.1–5 The “wiggles” seen, for example, in 3C449, NGC 6251, M87 and Cen A, may arise from helical instabilities.3,4 “Knots” may be radial oscillations (not necessarily unstable) forming sausage-like regions of compression, as in NGC 315, M87, Cen A etc. There seems no reason why such macroscopic modes should not appear. The smaller scale waves, however, cannot be easily resolved by radio astronomy, and can have profound effects, such as particle reacceleration. It would be rather more satisfying if there were observable large-scale implications of the microturbulence.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 97: Extragalactic Radio Sources , 1982 , pp. 231 - 232
Copyright
Copyright © Reidel 1982 

References

1. Ferrari, A., Trussoni, E., Zaninetti, L., Astr. Ap. 64, 43 (1978); Astr. Ap. 79, 190 (1979); Mon. Not. R.A.S. 193 469 (1980).Google Scholar
2. Benford, G., Ferrari, A., Trussoni, E., Ap. J. 241, 98 (1980).Google Scholar
3. Benford, G., Ap. J. 247, 458 (1981).CrossRefGoogle Scholar
4. Hardee, P. E., Ap. J. 234, 47 (1979).Google Scholar
5. Benford, G. and Cavallo, G., Astron. and Astrophys. 93, 171 (1981).Google Scholar