Abstract
In this chapter we discuss kiloparsec-scale AGN jets and their interactions with the environment, which lead to observed structures such as radio lobes and hotspots. After a brief summary of the history of the topic, we outline the basic physics of the emission processes, the sources’ key observational features (focussing on source physics) and their interpretation in terms of particle and field content, particle acceleration, and overall source dynamics.
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- 1.
It is conventional to talk about ‘the magnetic field strength in the lobes’ even though, in practice, we expect a strongly varying point-to-point magnetic field strength. We may define a mean field, \(B_{0}^{2} =\int B^{2}p(B)\mathrm{d}B\), and Hardcastle (2013) has shown in the case of a Gaussian random field with uniform electron energy density that the field estimates derived from inverse-Compton scattering of the CMB are effectively estimates of B 0. If there are also significant variations of the mean field strength from point to point in the lobe, as argued to be the case by e.g. Hardcastle and Croston (2005), then it is less clear what a lobe-averaged magnetic field strength means, but it seems likely that the values we measure are not far from a true lobe mean field strength.
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Acknowledgements
I am grateful to Robert Laing and Rick Perley for supplying radio images and Volker Gaibler for providing images from his numerical models. The NRAO VLA, with which all the radio images were made, is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.
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Hardcastle, M. (2015). Kiloparsec-Scale AGN Jets. In: Contopoulos, I., Gabuzda, D., Kylafis, N. (eds) The Formation and Disruption of Black Hole Jets. Astrophysics and Space Science Library, vol 414. Springer, Cham. https://doi.org/10.1007/978-3-319-10356-3_4
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