  Magnetic reconnection is a process of magnetic field topology change, which
is one of the most fundamental processes in magnetized plasmas. In most
astrophysical environments the Reynolds numbers are large and therefore the
transition to turbulence is inevitable. This turbulence must be taken into
account for any theory of magnetic reconnection, since the initially laminar
configurations can transit to the turbulence state, what is demonstrated by 3D
high resolution numerical simulations. We discuss ideas of how turbulence can
modify reconnection with the focus on the Lazarian & Vishniac (1999)
reconnection model and present numerical evidence supporting the model and
demonstrate that it is closely connected to the concept of Richardson diffusion
and compatible with the Lagrangian dynamics of magnetized fluids. We point out
that the Generalized Ohm's Law, that accounts for turbulent motion, predicts
the subdominance of the microphysical plasma effects for a realistically
turbulent media. We show that on of the most dramatic consequences of
turbulence is the violation of the generally accepted notion of magnetic flux
freezing. This notion is a corner stone of most theories dealing with
magnetized plasmas and therefore its change induces fundamental shifts in
accepted paradigms like turbulent reconnection entailing the diffusion process
that is essential for understanding star formation. We argue, that at
sufficiently high Reynolds numbers the process of tearing reconnection should
transfer to turbulent reconnection. We discuss flares predicted by turbulent
reconnection and relate them to solar flares and gamma ray bursts. We analyze
solar observations, measurements in the solar wind or heliospheric current
sheet, and show their correspondence with turbulent reconnection predictions.
Finally, we discuss 1st Order Fermi acceleration as a natural consequence of
the turbulent reconnection.
