Volume 442, Number 3, November II 2005
|Page(s)||1079 - 1086|
|Published online||14 October 2005|
The structure of a penumbral connection between solar pores
Institut für Physik, IGAM, Universitätsplatz 5, 8010 Graz, Austria
2 Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany e-mail: email@example.com
3 Astronomical Institute, Academy of Sciences of the Czech Republic, 25165 Ondřejov, Czech Republic
4 Universitäts-Sternwarte, Geismarlandstraße 11, 37083 Göttingen, Germany
Accepted: 17 June 2005
High resolution 2D-spectro-polarimetric observations have been used to analyse the magnetic field and flow topologies of a penumbral connection between two opposite polarity solar pores. A filamentary structured Evershed-like material flow from one pore to the other along the magnetic field lines has been detected. The flow channels are co-spatial with bright penumbral filaments close to the pore which feeds the flow and the clear brightness-velocity relation vanishes close to the pore which represents the sink of the flow. The boundary between umbra and penumbra of the two pores show significant differences: bright comet-like penumbral grains represent endings of penumbral filaments at the flow sources whereas no such grains were found at the sinks of the flow. Furthermore, a systematic variation of the asymmetries of measured Stokes V profiles across the penumbral connection have been found. The obtained results are in accordance with the widely-accepted uncombed penumbra hypothesis and the moving flux tube model.
Key words: Sun: photosphere / Sun: magnetic fields / Sun: sunspots
© ESO, 2005
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