Dynamics of the Solar Surface Reavealed by Granule Tracking

Details Dynamics of the Solar Surface Reavealed by Granule Tracking Dynamics of the Solar Surface Reavealed by Granule Tracking

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12..2.9r&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

We present the recent results obtained by the Toulouse-Tarbes group on the dynamics of the solar surface at meso and supergranular scale, and their interactions with the magnetic field.
First, using the 14-Mpixel CALAS camera at the Pic-du-Midi observatory, we obtained a 7.5h-long sequence of high resolution images with unprecedented field size (524"x350"). Tracking granules, we have determined the velocity field at the Sun's surface in great detail from a scale of 2.5 Mm up to 250 Mm. The kinetic energy density spectrum shows that supergranulation peaks at 36Mm and spans on scales ranging between 20Mm and 75Mm. The decrease of supergranular flows in the small scales is close to a 1/k^2-power law, steeper than the equipartition Kolmogorov one. The probability distribution function of the divergence field shows the signature of intermittency of the supergranulation and thus its turbulent nature.
Second, using a 48hours-long sequence of white light images from the HINODE satellite, we determined the evolution of granule families, which give birth to correlated motion at mesogranular scale. Using passive cork and magnetic field observations, we show that the surface velocity field via family organization is sufficient to explain the magnetic field concentrations at the Sun's surface, namely the magnetic network. We also find robust scaling laws for the life time of granule families.

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