My present scientific projects
The projects are sorted by my personal interest.
These pages are updated in general
monthly. They serve mainly to inform cooperating partners about the
status of our projects. They may also be used by interested colleagues
to gain information if they intend to join us in one or the other project.
In general you can get more details about scientific goals and
related findings of other research groups within the cited publications.
You may use the links of my publications.
In general you can get more details about scientific goals and related findings of other research groups within the cited publications. You may use the links of my publications.
A new observing run was performed end of August / begin of September 1998, again using the TESOS/FPI. The spectral lines used were again Fe 557.6 nm and for a first time Fe 630.25 nm. Unfortunately bad seeing conditions and technical problems did not allow to obtain useful data. Nevertheless these data are also used to check the reduction procedures. Further observations were performed in 1999: End of July the seeing was quite bad and no useful data could be obtained. End of August/begin of September 1999 we obtained several series with the spectral lines Fe 557.61 nm (non-split) and Cr 578.2 nm (strong splitting) in parallel. Within a further observing run begin of June 2000 due to instrumental problems and bad weather again no usefull data could be obtained. We plan to concentrate on further light-bridge studies in 2001/03. Another observing run in November/December 2002 was rather disappointing: Either the TESOS system was not yet running (a PLUTO PC had to be reconfigurated due to a new harddisk) or the wind did not blow from a nice direction and avoided any operation of the AO due to strange shaking of the coelostat/tower. Only a short sequence of data from November 27, 2002 is used to test the complete TESOS software for merging data (from the two CCDs) and data reduction.
In 2003 we used the Mercury transit to collect data to determine the scattered light in TESOS and some weeks later continued the observations again with Fe 557.6 nm and Cr 578.2 nm. For these observations the KAOS was in operation during all the data collections.
Further data were collected in 2001 and 2002 by V.Ruzdjak and also by myself in September/October 2002. Shown are two examples taken May 8, 2001 at Hvar and digitized September 5, 2001 at Freiburg. - Within the images are given: on top the 'Hvar-number' given to this group, in the left above the bottom line the directions on the sun (S=south, W=west, and a "L" for the symbol of the corner) and in the bottom line the date in YEAR-MONTH-DAY - format, the observing place ('HVAR') and the time in UT. After 'UT' the image number within the second shown is given (30 images per second).
If you want to know more about these projects, just ask me. You may use the e-mail connection below !