Physics
Scientific paper
Oct 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505...83s&link_type=abstract
In: SOLMAG 2002. Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188, 11 - 15 Jun
Physics
32
Sun, Magneto-Convection, Dynamo, Simulations
Scientific paper
Magneto-convection simulations on meso-granule and granule scales near the solar surface are used to study small scale dynamo activity and the emergence and disappearance of magnetic flux tubes. Convective motions produce highly intermittent magnetic fields in the intergranular lanes which collect over the boundaries of the underlying meso-granular scale cells. When observing these magnetic fields, it is important to note that the telescope point spread function and seeing significantly reduce the amplitudes of the observed Stokes profiles. Because of the strong stratification, there is little recycling of plasma and field in these surface layers. Recycling instead occurs by exchange with the deep layers of the convection zone. Plasma and field from the surface descend to the bottom of the convection zone, where they rise again toward the surface. Because the turnover time in the deep convection zone is of order a month, and because only a tiny fraction of plasma rising up from the bottom of the convection zone reaches the surface due to mass conservation, the time constant for this dynamo is long and 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.
Nordlund Åke
Stein Robert F.
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