Astronomical Institute
University of Wrocław
 
 
 
The Białkow Observatory is located in the country, on the outskirts of Białkow village, approximately 70 km north-west of Wrocław. The scientific staff works on solar flares and the photometry of variable stars.
 
 
 
The 60-cm Cassegrain Reflector
 
The technical details of the Cassegrain reflector:
          the main mirror's diameter:           600 mm
          the main mirror's focal length:     2400 mm
          the secondary mirror's diameter:   183 mm
          the equivalent focal length:          7500 mm
          the field of view:                            20'
 
Our reflector is equipped with a CCD camera and Johnson-Cousins, Strömgren and  Hα sets of filters. Our main photometric targets are open clusters (searching for B-type variable stars) and globular clusters (e.g. RR Lyrae-type stars).
 
Observers: A. Pigulski, G. Kopacki, A. Majewska, D. Drobek, A. Narwid, M. Stęślicki and E. Niemczura.
 
 
 
The 53-cm Coronograph
In Białkow Observatory we have two solar telescopes: Large Coronagraph (LC) and Horizontal Telescope (HT). The observatory is equipped also with Multi-Channel Subtractive Double Pass spectrograph (MSDP-spectrograph) (Mein,1991; Rompolt et al, 1994 ).
 
The LC has a 53 cm diameter main objective, its effective focal length is 14.5 m, and spatial resolution, normally limited by seeing conditions, about 1 arcsec or better. The LC could be use as coronagraph as well as chromospherograph - the observations of solar surface (solar chromosphere) covering usually more then 90 percent of observational time. Second (auxiliary) instrument is Horizontal Telescope with a compact Jensch-type coelostat. The main objective of HT has an aperture of 15 cm and focal length 5 m.
 
The MSDP imaging-spectrograph has a rectangular entrance window, which covers (for LC) an equivalent area of 325 x 41 arcsec2 on the Sun. The MSDP spectrograph has a nine-channel "prism-box", enabling restoration of the Hα line profiles (in each pixel of image) in the range about ± 1.2 Å from the line centre using the emission measured in nine wavelengths separated by 0.4 Å. The spectra-images created by the MSDP spectrograph could be recorded in slow mode (with scanner) or in fast mode by the use Solar Eclipse Coronal Imaging System (SECIS). The SECIS instrument was originally designed and used by British-Polish expeditions for investigation of fast intensity changes in solar coronal features during the total solar eclipses (Phillips et al, 2000). Slow mode of observations enable to obtain spectral-images with time resolution about 20-45 s, however the fast mode reach the time resolution 0.04-0.075 s.
 
The main subjects of observations in our observatory are solar flares (e.g.: Rudawy et al, 2001) - in last few years mainly fast changes of emission in the range of Hα (6562.8 Å) line (e.g.: Radziszewski et al, 2007). The prominences, filaments and plasma eruptions are also observed.
 
Observers: P. Rudawy, A. Berlicki, K. Radziszewski and B. Rompolt (retaired).
About the Observatory