Reconnection in turbulent astrophysical fluids
  Magnetic reconnection is a fundamental process of magnetic field topology
change. We analyze the connection of this process with turbulence which is
ubiquitous in astrophysical environments. We show how Lazarian & Vishniac
(1999) model of turbulent reconnection is connected to the experimentally
proven concept of Richardson diffusion and discuss how turbulence violates the
generally accepted notion of magnetic flux freezing. We note that in
environments that are laminar initially turbulence can develop as a result of
magnetic reconnection and this can result in flares of magnetic reconnection in
magnetically dominated media. In particular, magnetic reconnection can
initially develop through tearing, but the transition to the turbulent state is
expected for astrophysical systems. We show that turbulent reconnection
predictions corresponds to the Solar and solar wind data.
