2009 Hovatta, T. AGN的Lorentz因子和观测角

主要内容:
AGN中的radio quasar和BL Lac天体。
Lorentz因子基本上是10左右半个量级。

通过variability定的Lorentz因子，原理待细究。

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Title:		Doppler factors, Lorentz factors and viewing angles for quasars, BL Lacertae objects and radio galaxies [ Erratum: 2009A&A...498..723H ]
Authors:		Hovatta, T.; Valtaoja, E.; Tornikoski, M.; Lähteenmäki, A.
Affiliation:		AA(Metsähovi Radio Observatory, TKK, Helsinki University of Technology, Metsähovintie 114, 02540 Kylmälä, Finland tho@kurp.hut.fi), AB(Tuorla Observatory, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland; Department of Physics and Astronomy, University of Turku, Vesilinnantie 5, 20100 Turku, Finland), AC(Metsähovi Radio Observatory, TKK, Helsinki University of Technology, Metsähovintie 114, 02540 Kylmälä, Finland), AD(Metsähovi Radio Observatory, TKK, Helsinki University of Technology, Metsähovintie 114, 02540 Kylmälä, Finland)
Publication:		Astronomy and Astrophysics, Volume 494, Issue 2, 2009, pp.527-537 (A&A Homepage)
Publication Date:		02/2009
Origin:		EDP Sciences
Astronomy Keywords:		galaxies: active, galaxies: jets, radio continuum: galaxies, radiation mechanisms: non-thermal, galaxies: quasars: general
DOI:		10.1051/0004-6361:200811150
Bibliographic Code:		2009A&A...494..527H

Abstract

Aims: We have calculated variability Doppler boosting factors, Lorentz factors, and viewing angles for a large sample of sources by using total flux density observations at 22 and 37 GHz and VLBI data.
Methods: We decomposed the flux curves into exponential flares and determined the variability brightness temperatures of the fastest flares. By assuming the same intrinsic brightness temperature for each source, we calculated the Doppler boosting factors for 87 sources. In addition we used new apparent jet speed data to calculate the Lorentz factors and viewing angles for 67 sources.
Results: We find that all quasars in our sample are Doppler-boosted and that the Doppler boosting factors of BL Lacertae objects are lower than of quasars. The new Lorentz factors are about twice as high as in earlier studies, which is mainly due to higher apparent speeds in our analyses. The jets of BL Lacertae objects are slower than of quasars. There are some extreme sources with very high derived Lorentz factors of the order of a hundred. These high Lorentz factors could be real. It is also possible that the sources exhibit such rapid flares that the fast variations have remained undetected in monitoring programmes, or else the sources have a complicated jet structure that is not amenable to our simple analysis. Almost all the sources are seen in a small viewing angle of less than 20 degrees. Our results follow the predictions of basic unification schemes for AGN.

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