Abstract
AbstractRelations between horizontal flow and filigree structure obtained from high-resolution observations (~1/4) are discussed. The magnetic flux elements move with the horizontal flow in the supergranulation network, and as downdrafts are approached both magnetic flux and intensity gradually decrease. Reasons for this disappearance are discussed. If the photosphere actually is a turbulent magneto-plasma, as suggested by the good coupling between the magnetic flux elements and the flow field, the integrated magnetic flux in the background field will exceed the flux in the discrete kilogauss structures.
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