Statistics – Computation
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...284..724c&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 284, no. 3, p. 724-730
Statistics
Computation
15
Linear Polarization, Quasars, Radio Astronomy, Radio Jets (Astronomy), Relativistic Velocity, Shock Fronts, Synchrotron Radiation, Computation, Doppler Effect, Mach Number, Nonthermal Radiation, Numerical Analysis
Scientific paper
The jet of 3C 273 is interpreted as synchrotron plasma moving at a mildly relativistic speed up to a terminal shock, identified with the brightest radio component, H2, in the head. The Mach number of the flow can be deduced from the brightness contrast of the shocked gas compared with the upstream portions of the flow, after making due allowance for the effects of the Doppler beaming. This shows that the jet speed is approximately equals 0.8 c, while the speed of the shocked gas is approximately equals 0.4 c. By comparing the linear polarization of the jet (18%, with B parallel to the jet axis), and that of the shocked gas (23% with B transverse), it is shown that the direction of the jet must be 30 deg - 35 deg to the line of sight. The Doppler shift of the shocked gas in the head is less than or equal to 1.5, and is insufficient to hide a hypothetical counter-jet by a factor of about 2000. The direction of the jet differs by 20 deg - 30 deg from that deduced from the superluminal proper motion detected in the core, most probably because of a bend situated at a distance between 8 and 20 mas from the core. We suggest that the virtual absence of optical emission from H2 can be explained if there has been a recent disconnection event, as suggested by the 'Dentist's Drill' model of Cox, Gull & Scheuer.
Conway R. G.
Davis Raymond Jr.
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