  Spatial intermittency in decaying kinetic Alfven wave turbulence is
investigated to determine if it produces non Gaussian density fluctuations in
the interstellar medium. Non Gaussian density fluctuations have been inferred
from pulsar scintillation scaling. Kinetic Alfven wave turbulence characterizes
density evolution in magnetic turbulence at scales near the ion gyroradius. It
is shown that intense localized current filaments in the tail of an initial
Gaussian probability distribution function possess a sheared magnetic field
that strongly refracts the random kinetic Alfven waves responsible for
turbulent decorrelation. The refraction localizes turbulence to the filament
periphery, hence it avoids mixing by the turbulence. As the turbulence decays
these long-lived filaments create a non Gaussian tail. A condition related to
the shear of the filament field determines which fluctuations become coherent
and which decay as random fluctuations. The refraction also creates coherent
structures in electron density. These structures are not localized. Their
spatial envelope maps into a probability distribution that decays as density to
the power -3. The spatial envelope of density yields a Levy distribution in the
density gradient.
