  Magneto-convection simulations on meso-granule and granule scales near the
solar surface are used to study small scale dynamo activity, the emergence and
disappearance of magnetic flux tubes, and the formation and evolution of
micropores.
  From weak seed fields, convective motions produce highly intermittent
magnetic fields in the intergranular lanes which collect over the boundaries of
the underlying meso-granular scale cells. Instances of both emerging magnetic
flux loops and magnetic flux disappearing from the surface occur in the
simulations. We show an example of a flux tube collapsing to kG field strength
and discuss how the nature of flux disappearance can be investigated. Observed
stokes profiles of small magnetic structures are severely distorted by
telescope diffraction and seeing.
  Because of the strong stratification, there is little recycling of plasma and
field in the surface layers. Recycling instead occurs by exchange with the deep
layers of the convection zone. Plasma and field from the surface descend
through the convection zone and rise again toward the surface. Because only a
tiny fraction of plasma rising up from deep in the convection zone reaches the
surface due to mass conservation, little of the magnetic energy resides in the
near surface layers. Thus the dynamo acting on weak incoherent fields is
global, rather than a local surface dynamo.
