  Magnetic reconnection in partially ionized plasmas is a ubiquitous phenomenon
spanning the range from laboratory to intergalactic scales, yet it remains
poorly understood and relatively little studied. Here, we present results from
a self-consistent multi-fluid simulation of magnetic reconnection in a weakly
ionized reacting plasma with a particular focus on the parameter regime of the
solar chromosphere. The numerical model includes collisional transport,
interaction and reactions between the species, and optically thin radiative
losses. This model improves upon our previous work in Leake et al. 2012
\cite{Leake2012} by considering realistic chromospheric transport coefficients,
and by solving a generalized Ohm's law that accounts for finite ion-inertia and
electron-neutral drag.
  We find that during the two dimensional reconnection of a Harris current
sheet with an initial width larger than the neutral-ion collisional coupling
scale, the current sheet thins until its width becomes less than this coupling
scale, and the neutral and ion fluids decouple upstream from the reconnection
site. During this process of decoupling, we observe reconnection faster than
the single-fluid Sweet-Parker prediction, with recombination and plasma outflow
both playing a role in determining the reconnection rate.
  As the current sheet thins further and elongates it becomes unstable to the
secondary tearing instability, and plasmoids are seen. The reconnection rate,
outflows and plasmoids observed in this simulation provide evidence that
magnetic reconnection in the chromosphere could be responsible for jet-like
transient phenomena such as spicules and chromospheric jets.
