Doppler Boosting, Superluminal Motion, and the Kinematics of AGN Jets

Details Doppler Boosting, Superluminal Motion, and the Kinematics of AGN Jets Doppler Boosting, Superluminal Motion, and the Kinematics of AGN Jets

2007-08-23

arxiv.org/abs/0708.3219v1

Astrophys.SpaceSci.311:231-239,2007

Astronomy and Astrophysics

Astrophysics

10 pages, 12 color figures; proceedings of the 5th Stromlo Symposium: Disks, Winds, and Jets - from Planets to Quasars; accept

Scientific paper

10.1007/s10509-007-9622-5

We discuss results from a decade long program to study the fine-scale structure and the kinematics of relativistic AGN jets with the aim of better understanding the acceleration and collimation of the relativistic plasma forming AGN jets. From the observed distribution of brightness temperature, apparent velocity, flux density, time variability, and apparent luminosity, the intrinsic properties of the jets including Lorentz factor, luminosity, orientation, and brightness temperature are discussed. Special attention is given to the jet in M87, which has been studied over a wide range of wavelengths and which, due to its proximity, is observed with excellent spatial resolution. Most radio jets appear quite linear, but we also observe curved non-linear jets and non-radial motions. Sometimes, different features in a given jet appear to follow the same curved path but there is evidence for ballistic trajectories as well. The data are best fit with a distribution of Lorentz factors extending up to gamma ~30 and intrinsic luminosity up to ~10^26 W/Hz. In general, gamma-ray quasars may have somewhat larger Lorentz factors than non gamma-ray quasars. Initially the observed brightness temperature near the base of the jet extend up to ~5x10^13 K which is well in excess of the inverse Compton limit and corresponds to a large excess of particle energy over magnetic energy. However, more typically, the observed brightness temperatures are ~2x10^11 K, i.e., closer to equipartition.

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