  We have calculated inverse-Compton Doppler factors for 3C 279 using the
collection of VLBI data recently published by us, and the collection of
multiwavelength spectra recently published by Hartman et al. From the Doppler
factor and superluminal apparent speed, we then calculate the Lorentz factor
and angle to the line-of-sight of the parsec-scale relativistic jet. We model
the jet components as homogeneous spheres and the VLBI core as an unresolved
inhomogeneous conical jet. The conical-jet model can be made to match both the
observed X-ray emission and the VLBI properties of the core with a suitable
choice of Doppler factor, implying the core makes a significant contribution to
the X-ray emission. The parameters of the conical models indicate the jet is
particle dominated at the radii that produce significant emission, and is not
in equipartition. At the inner radius of the conical jet the magnetic field is
of order 0.1 G and the relativistic-particle number density is of order 10
cm^{-3}. When all components are included in the calculation, then on average
the core produces about half of the X-rays, with the other half being split
between the long-lived component C4 and the brightest inner-jet component. We
calculate an average speed and angle to the line-of-sight for the region of the
jet interior to 1 mas of v=0.992c (gamma=8) and 4 degrees, and an average speed
and angle to the line-of-sight for C4 (at a distance from the core of 3 mas) of
v=0.997c (gamma=13) and 2 degrees. These values imply average Doppler factors
of delta=12 for the inner jet, and delta=21 for C4.
