Contents List of Figures

294 6 MACRO– AND MICRO–JETS DRIVEN BY BLACK HOLES
von Montigny et al. (1997) examined 3 models to reproduce the multifrequency
spectrum of 3C 273: (i) the synchrotron–self Compton model (SSC model); (ii) the
external radiation Compton model (ERC model; Sikora, Begelman and Rees 1994),
and, (iii) the proton induced cascade model (PIC model; Mannheim & Biermann
1992). At that time, the authors concluded that the data were still insufficient to
discriminate between the models. In Fig. 141, a simple one–zone model is shown to
explain the spectrum. In this simple model, the radiation is due to a homogeneous
jet component moving with a bulk Lorentz factor ΓBLK at an angle of line of sight
Θ 1/ΓBLK. It is assumed that the peak emission of the low–energy synchrotrn
component (LE) and the high energy inverse Compton components (HE) arise from
the same electron population with Lorentz factor γp. The peak frequencies of LE
and HE are related by
νHE,p = 4
(706)
3 γ2 pνLE,p
with νLE,p = 10 13.5 Hz, and νHE,p = 10 20 Hz. This requires a γp = 2 × 10 3 . The
Figure 141: Global spectrum for 3C 273 with X–rays as explained by SSC–emission
(Katakoa et al. 2002).
synchrotron peak frequency νLE,p is given by
νLE,p = 3.7 × 10 6 B γ 2 p
D
Hz (707)
1 + z