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Astron. Astrophys. 334, 427-438 (1998)

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4. Conclusions

We considered the dynamics of the groups of galaxies around 3C 275.1. Basing upon criterion " [FORMULA] " we realized that only five galaxies from the lists published by Hintzen (1984) and Ellingson and Yee (1994) are dynamically bound with the quasar. It is worth noting that the host galaxy of quasar with its low radial velocity in respect to the group, i.e. [FORMULA], resides in the bottom of gravitational potential well of the group. Accordingly, its relative motion through the ICM gas cannot explain the non-collinearity of the radio structure of the quasar. We proposed that the oblique shock of radio jet at the interface with the halo of the neighboring galaxy "381" or with knots of ionized gas emitting the forbidden narrow-emission lines might be responsible for the deflection of counter-jet. The knots of the ionized gas can be produced by the cooling flow with the deposition mass rate of the order of [FORMULA]. Then, the calculated number and mass densities in such knots of the size of 10 [FORMULA] are about [FORMULA] and about [FORMULA] respectively. To explain the deflection angle of [FORMULA] we consider two cases of oblique shocks. In the first case the flow velocities and the magnetic fields are parallel to each other in upstream and downstream flows, while in the second one the magnetic field become perpendicular to flow velocities after the shock. We derived the relation between the angle [FORMULA] and the angle between the upstream flow velocity [FORMULA] and the normal to the discontinuity surface as the functions of the ratios of gas "a" and of magnetic " [FORMULA] " pressures. For observed ratios of magnetic field pressures [FORMULA], of gas pressures a=1.6, the upstream gas pressure [FORMULA] and [FORMULA] we derived the angles between the upstream velocity and normal to surface shock [FORMULA] and between the surface shock and the line of sight [FORMULA] equal to [FORMULA] and [FORMULA] respectively. We also calculated the conditions for upstream velocity [FORMULA] and [FORMULA].

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© European Southern Observatory (ESO) 1998

Online publication: May 15, 1998

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