  We use a combination of high-resolution very long baseline interferometry
(VLBI) radio and multi-wavelength flux density and polarization observations to
constrain the physics of the dissipation mechanism powering the broadband
flares in 3C 279 during an episode of extreme flaring activity in 2013-2014.
Six bright flares superimposed on a long-term outburst are detected at
$\gamma$-ray energies. Four of the flares have optical and radio counterparts.
The two modes of flaring activity (faster flares sitting on top of a long term
outburst) present at radio, optical, $\gamma$-ray frequencies are missing in
X-rays. X-ray counterparts are only observed for two flares. The first three
flares are accompanied by ejection of a new VLBI component (NC2) suggesting the
43 GHz VLBI core as the site of energy dissipation. Another new component, NC3,
is ejected after the last three flares, which suggests that the emission is
produced upstream from the core (closer to the black hole). The study therefore
indicates multiple sites of energy dissipation in the source. An
anti-correlation is detected between the optical percentage polarization (PP)
and optical/$\gamma$-ray flux variations, while the PP has a positive
correlation with optical/$\gamma$-rays spectral indices. Given that the mean
polarization is inversely proportional to the number of cells in the emission
region, the PP vs. optical/$\gamma$-ray anti-correlation could be due to more
active cells during the outburst than at other times. In addition to the
turbulent component, our analysis suggests the presence of a combined turbulent
and ordered magnetic field, with the ordered component transverse to the jet
axis.

High Energy Astrophysical Phenomena