Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994arep...38..617k&link_type=abstract
Astronomy Reports, Volume 38, Issue 5, September 1994, pp.617-623
Astronomy and Astrophysics
Astronomy
Scientific paper
Asymmetries observed in double extended radio sources are considered: asymmetries in radio component positions, radiojet direction, averaged depolarization of radiation, extended emission regions, and mean spectral indices. Causes of asymmetries discussed earlier in the literature are analyzed: a nonhomogeneous Faraday screen with randomly oriented cells of a homogeneous magnetic field in hot intergalactic gas; nonhomogeneous distribution of matter around an active nucleus, which results in differing dissipation of a jet and counterjet; intrinsic differences in the properties of a jet and counterjet (in energy, velocity, lifetime). It is shown that observed asymmetries can be understood in the framework of a "flip-flop"-type model of jets with certain relationships between temporal parameters. The asymmetry of extended components is due to the age difference and, as a consequence, to different quantities of gas swept by the jets. Attention is given to the possible role of cooling flows in the formation of asymmetries in double radio sources in central regions of rich clusters of galaxies. The presence of cooling flows may account for the assignment of type FRII and FRI double radio source to the "giant sequence" and "main sequence" (in Shklovskii's terms), respectively. For an active galactic nucleus, a model of a massive binary system with counterrotation of the components is suggested. The reverse in jet direction can be obtained if a binary is embedded in a thick disk whose plane coincides with the direction of component rotation axes and is perpendicular to the plane of component rotation. Developing Shklovskii's idea on the influence of recoil momentum of a one-sided, powerful jet upon the nucleus, we predict the possibility of active nucleus oscillation with a period of 10^6^ - 10^7^ years on scales of several kiloparsecs. Some features of quasar 3C 48 may be due to this effect.
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