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Quasi-Two-Dimensional Cosmic Jets

Published online by Cambridge University Press:  04 August 2017

K. Tsinganos ,
A. Ferrari  and
R. Rosner
K. Tsinganos
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
A. Ferrari
Affiliation:
Istituto di Fisica Generale, Universita di Torino, 1-10125 Torino, ITALY
R. Rosner
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA

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One of the major discoveries in solar physics over the past decade has been the association of coronal holes with high-speed solar wind streams (Zirker 1977 and references therein). On the other hand, advances in X-ray and radio instrumentation (e.g., Einstein, VLA, VLBI, etc.) in the past few years have allowed detailed observations of collimated outflows from rather more distant objects, such as young stars and active galaxies (Beer 1981, Lada 1982, Ferrari and Pacholczyk 1983 and references therein). The remarkable structural similarities between jets of magnetized gas from our Sun, other active stars, and active galactic nuclei suggest that these phenomena may be manifestations of similar hydrodynamic processes operating on both small and large scales. In this article, we shall use the experience gained by studying the nearest known astrophysical jet - high-speed solar wind streams - to address some of the problems of astrophysical jet acceleration and collimation associated with objects as diverse as SS 433, star-forming molecular clouds and, in particular, jets associated with galaxies and quasars.

Type
Session VII
Information
Symposium - International Astronomical Union , Volume 107: Unstable Current Systems and Plasma Instabilities , 1985 , pp. 497 - 501
Copyright
Copyright © Reidel 1985 

References

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