Modeling the 3C 120 Radio Jet from 1 to 30 Milliarcseconds

Details Modeling the 3C 120 Radio Jet from 1 to 30 Milliarcseconds Modeling the 3C 120 Radio Jet from 1 to 30 Milliarcseconds

2004-10-29

arxiv.org/abs/astro-ph/0410720v1

Astrophys.J. 620 (2005) 646-664

Astronomy and Astrophysics

Astrophysics

26 pages, 15 figures, in press Astrophysical Journal

Scientific paper

10.1086/427083

The predicted spatial development of helical structures along an expanding jet are used to model observed structures and motions in the 3C 120 jet. Proper motions of helical components associated with the pattern and of other components that move through the pattern provide estimates of flow and helical pattern speeds. Theoretical modeling allows determination of sound speeds as a function of jet viewing angle. Jet morphology argues against viewing angles larger than 12 deg. At a 12 deg viewing angle the most likely scenario involves a decline in jet sound speed from c/3 < a_j < c/1.7 at ~0.5 mas from the core to 0.1c < a_j < 0.25c at ~25 mas from the core accompanied by some acceleration in the jet flow from Lorentz factor < 5 to Lorentz factor > 7. At smaller viewing angles the jet sound speed is lower and at a 6 deg viewing angle the jet sound speed is about a factor 2 less but the flow Lorentz factor is comparable. The decline in radio intensity is on the order of what would be associated with isothermal jet expansion. Knot interknot intensity variations are greater than would be expected from adiabatic compressions associated with the helical twist and we infer the presence of a shock along the leading edge of the helical twist. Our results imply that the macroscopic heating of the expanding jet fluid is less than the microscopic energization of the synchrotron radiating relativistic electrons.

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