Abstract
Collimated outflows (jets) appear to be a ubiquitous phenomenon associated with the accretion of material onto a compact object. Despite this ubiquity, many fundamental physics aspects of jets are still poorly understood and constrained. These include the mechanism of launching and accelerating jets, the connection between these processes and the nature of the accretion flow, and the role of magnetic fields; the physics responsible for the collimation of jets over tens of thousands to even millions of gravitational radii of the central accreting object; the matter content of jets; the location of the region(s) accelerating particles to TeV (possibly even PeV and EeV) energies (as evidenced by \(\gamma\)-ray emission observed from many jet sources) and the physical processes responsible for this particle acceleration; the radiative processes giving rise to the observed multi-wavelength emission; and the topology of magnetic fields and their role in the jet collimation and particle acceleration processes. This chapter reviews the main knowns and unknowns in our current understanding of relativistic jets, in the context of the main model ingredients for Galactic and extragalactic jet sources. It discusses aspects specific to active Galactic nuclei (especially blazars) and microquasars, and then presents a comparative discussion of similarities and differences between them.
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Notes
Henceforth, we refer to as “comoving” or “jet frame” the reference frame fixed to the jet plasma, where the outflow bulk velocity is zero. The “observer frame” corresponds to the frame in which the jet bulk velocity is \(v_{\mathrm{{jet}}}\).
Note a typo in Eqs. (3.38) and (3.39) in Böttcher et al. (2012), where a factor \(c\) is missing
For simplicity we are assuming that the clouds producing the broad lines are located at the same distance. In reality, different emission lines are likely produced in a stratified BLR, in which the ionization factor decreases with distance (Netzer 2008).
The other one is Cygnus X-3.
Any opinion, finding and conclusion or recommendation expressed in this material is hat of the authors, and the NRF does not accept any liability in this regard.
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Acknowledgements
We would like to thank the ISSI staff for providing an inspiring atmosphere favorable for intense discussions. GER thanks support from CONICET (PIP 2014-0338) and grant AYA2016-76012-C3-1-P (Ministro de Educación, Cultura y Deporte, Spain). The work of M.B. is supported by the South African Research Chairs Initiative (SARChI) of the Department of Science and Technology and the National Research FoundationFootnote 5 of South Africa, under SARChI Chair grant No. 64789.
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Romero, G.E., Boettcher, M., Markoff, S. et al. Relativistic Jets in Active Galactic Nuclei and Microquasars. Space Sci Rev 207, 5–61 (2017). https://doi.org/10.1007/s11214-016-0328-2
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DOI: https://doi.org/10.1007/s11214-016-0328-2