Physics
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.2.28s&link_type=abstract
"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,
Physics
1
Scientific paper
A sunspot is a coherent phenomenon on large spatial and temporal scales, but it consists of an ensemble of small-scale and dynamic features. It seems crucial to realize that a sunspot is not static, but manifests a dynamic equilibrium: The dynamic fine structure forms a globally stable sunspot, and it is the goal of sunspot physics to understand how an ensemble of short living features on small scales is organized to form a coherently large and long living sunspot. To this end it is a necessity to investigate the nature of the fine structure: its small-scale flow field, the topology of the magnetic field, and the radiative interactions that form the intensity fine structure. We know that the energy transport has to be of convective nature, but up to now the underlying convective processes remain unclear. Is it convection in magnetic field free gaps that exist in the space separating a strong magnetic field which is more or less static? Is it convective flows that are channeled by magnetic flux tube? Or is it dissipative turbulent magneto-convection?
In this contribution we study the small-scale flow field in order to learn about the convective flow pattern. We take advantage of the high spatial and high spectral resolution data from Hinode. The satellite has acquired spectroscopic data from disk passages of about 10 sunspots in 2007. Taking into account the varying viewing angle according to the location of the sunspot on the disk, we investigate the small-scale flow pattern. Thereby, we aim at an understanding of the type of convection that is responsible for the Evershed flow, for the small-scale penumbral structure, and for the energy transport in penumbrae.
Franz Marcel
Schlichenmaier Rolf
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