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Energetic and Broad Band Spectral Distribution of Emission from Astronomical Jets

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Abstract

Emission from astronomical jets extend over the entire spectral band: from radio to the TeV γ-rays. This implies that various radiative processes are taking place in different regions along jets. Understanding the origin of the emission is crucial in understanding the physical conditions inside jets, as well as basic physical questions such as jet launching mechanism, particle acceleration and jet composition. In this chapter I discuss various radiative mechanisms, focusing on jets in active galactic nuclei (AGN) and X-ray binaries (XRB) environment. I discuss various models in use in interpreting the data, and the insights they provide.

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Notes

  1. Jet dominated models are expected in XRBs during the low/hard state, where L∼1 %L Edd. At higher luminosities, disk contribution is expected, and the spectral slope varies; the luminosity-dependence of the spectral index can be found in Wu and Gu (2008).

  2. Data taken from McClintock et al. (2001); Note, though, that a different analysis of BeppoSAX (Frontera et al. 2001) and Chandra (Reis et al. 2009) data done in the context of disk models, resulted in a somewhat softer slope below 2 keV.

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Acknowledgements

I would like to thank Paul Callanan, Piergiorgio Casella, Amir Levinson and Abraham Loeb for providing useful comments on this manuscript.

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    Asaf Pe’er

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Pe’er, A. Energetic and Broad Band Spectral Distribution of Emission from Astronomical Jets. Space Sci Rev 183, 371–403 (2014). https://doi.org/10.1007/s11214-013-0001-y

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