  Order of magnitude variability has been observed in the blazar sub-class of
Active Galactic Nuclei on minute timescales. These high-energy flares are often
difficult to explain with shock acceleration models due to the small size of
the inferred emitting region, with recent particle-in-cell (PIC) simulations
showing that magnetic reconnection is a promising alternative mechanism. Here,
we present a macroscopic emission model physically motivated by PIC
simulations, where the energy for particle acceleration originates from the
reconnecting magnetic field. We track the radial growth and relative velocity
of a reconnecting plasmoid, modelling particle acceleration and radiative
losses from synchrotron and synchrotron self-Compton (SSC) emission. To test
the viability of magnetic reconnection as the mechanism behind rapid blazar
flares we simultaneously fit our model to the observed light-curve and SED from
the 2016 TeV flare of BL Lacertae. We find generally that, without considering
external photons, reconnecting plasmoids are unable to produce Compton-dominant
TeV flares and so cannot reproduce the observations due to overproduction of
synchrotron emission. Additionally, problematically large plasmoids, comparable
in size to the entire jet radius, are required to emit sufficient SSC
gamma-rays to be observable. However, our plasmoid model can reproduce the
rapid TeV lightcurve of the flare, demonstrating that reconnection is able to
produce rapid, powerful TeV flares on observed timescales. We conclude that
while reconnection can produce SSC flares on the correct timescales, the
primary source of TeV emission cannot be SSC and the size of plasmoids required
may be implausibly large.
