Dynamical Models for Jet Deceleration
in the Radio Galaxy 3C31

R.A.Laing Space Science and Technology Department, CLRC, Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX and University of Oxford, Department of Astrophysics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH A.H.Bridle National Radio Astronomy Observatory 520 Edgemont Road, Charlottesville, VA 22903-2475, U.S.A. Monthly Notices of the Royal Astronomical Society, in press

3C31: Radio jets at 3.6cm (red) on WFPC2 optical image (blue)

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Abstract:

We present a dynamical analysis of the flow in the jets of the low-luminosity radio galaxy 3C31 based on our earlier geometrical and kinematic model (Laing and Bridle 2002) and on estimates of the external pressure and density distributions from Chandra observations (Hardcastle et al. 2002). We apply conservation of particles, energy and momentum to derive the variations of pressure and density along the jets and show that there are self-consistent solutions for deceleration by injection of thermal matter. We initially take the jets to be in pressure equilibrium with the external medium at large distances from the nucleus and the momentum flux to be = /c, where is the energy flux; we then progressively relax these constraints. With our initial assumptions, the energy flux is well determined: 9 -- 14 x 10³⁶ W. We infer that the jets are over-pressured compared with the external medium at the flaring point (1.1 kpc from the nucleus) where they start to expand rapidly. Local minima in the density and pressure and maxima in the mass injection rate and Mach number occur at 3 kpc. Further out, the jets decelerate smoothly with a Mach number 1. The mass injection rate we infer is comparable with that expected from stellar mass loss throughout the cross-section of the jet close to the flaring point, but significantly exceeds it at large distances. We conclude that entrainment from the galactic atmosphere across the turbulent boundary layer of the jet is the dominant mass input process far from the nucleus, but that stellar mass loss may also contribute near the flaring point. The occurrence of a significant over-pressure at the flaring point leads us to suggest that it is the site of a stationary shock system, perhaps caused by reconfinement of an initially free jet. Our results are compatible with a jet consisting of e^-e⁺ plasma on parsec scales which picks up thermal matter from stellar mass loss to reach the inferred density and mass flux at the flaring point, but we cannot rule out an e^-p⁺ composition with a low-energy cut-off.