Freiburg 2008 – scientific programme
Parts | Days | Selection | Search | Downloads | Help
EP: Fachverband Extraterrestrische Physik
EP 7: The Sun and Heliosphere I
EP 7.6: Talk
Tuesday, March 4, 2008, 15:45–16:00, KGI-Aula
Solar wind outflow from the base of the corona: Comparison of modeled EUV spectra and observations — •Pia Zacharias1, Hardi Peter1, and Jörg Büchner2 — 1Kiepenheuer-Institut für Sonnenphysik, Freiburg, Germany — 2Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
It is generally agreed upon that the fast solar wind originates from (polar) coronal holes. It is still under discussion, however, from which structures within the hole the wind is coming and how the mass is supplied to the wind. In the past, it was mostly assumed that there is a continuous outflow from the chromosphere through the transition region and corona into the wind. In contrast to this, observations of Tu et al (2005; Sci 308, 519) showed first indications that the mass to the wind is supplied into coronal funnels at a height in the corona corresponding to the transition region at a couple of 100.000 K. In this presentation we will examine 3D MHD models of a part of a coronal hole in terms of the EUV emission line spectra. We compare these results to actual observations in order to test the new suggestion of mass supply to the wind above the transition region.