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Magnetic energy and helicity fluxes at the photospheric level View all abstracts by submitter

Pascal Demoulin   Submitted: 2003-04-24 09:42

The source of coronal magnetic energy and helicity lies below the surface of the sun, probably in the convective zone dynamo. Measurements of magnetic and velocity fields can capture the fluxes of both magnetic energy and helicity crossing the photosphere. We point out the ambiguities which can occur when observations are used to compute these fluxes. In particular, we show that these fluxes should be computed only from the horizontal motions deduced by tracking the photospheric cut of magnetic flux tubes. These horizontal motions include the effect of both the emergence and the shearing motions what ever the magnetic configuration complexity is. We finally analyze the observational difficulties involved in deriving such fluxes, in particular the limitations of the correlation tracking methods.

Authors: Demoulin, P., Berger, M.A.
Projects: Soho-MDI

Publication Status: Solar Physics, in press
Last Modified: 2003-04-24 09:45
Go to main E-Print page  Helicity Transport and Generation in the Solar Convection Zone  MAGNETIC HELICITY CHANGES OF SOLAR ACTIVE REGIONS  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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