Astronomical Institute and Slovak Astronomical Society of the Slovak Academy of Sciences will continue in observing of the solar corona during the August 11, 1999 solar eclipse. The eclipse team will be splitted and located along the path of totality due the weather condition. Scientific program will be as follow:
Photometry and structure of the inner white-light corona
Equipment: A 20 cm lens with a focal length of 300 cm. The lens will be fed by a light from a 35 cm coelostat mirror. Several frames will be taken on a plane film of 18 x 24 cm with a short and longer exposures. It is supposed to take the solar corona picture up to 3 solar radii without of a neutral radial-gradded filter due a possibility of computer image-processed technique.
Photometry and structure of the outer white-light corona
Telelens a 8/500 mm will be used to take the solar corona with different exposures on the colour film.
Observational site: Elazig (Harput), 38 degrees and 42 arcmin N, 39 degrees and 15 arcmin E,Turkey
Participants: V. Rusin (head), P. Zimmermann, L. Klocok, M. Minarovjech
These experiments will be collaborated to Kandilli Observatory team headed by Dr. A. Ozguc (Turkey) and Kitt Peak Observatory team, headed by Dr. B. Livingston.
Two a 10 cm lenses, F = 100 (200) cm will be used to take several snapshots in the white-light up to 4-5 solar radii. Colour film will be used.
Place: Hungary (different observational sites)
Responsible persons: Dr. J. Ziznovsky, Dr. E Pittich
Spectrum of the solar corona
Target: Two snapshots of the corona spectrum in the spectral range of 480 nm to 570 nm with a dispersion of 1 nm/mm wil be taken. The first one will be taken with a slit tangentially oriented to the solar surface at the height of 1.5 solar radii. The snapshot will be taken immediately after the second contact. The second one, the slit will intersect the Moon and the spectrum will be taken in two oposite spaces in the solar corona. These material will be used
(1) to study a presence of chromospheric lines in the corona
(2) to separate an emission of the K- and F-corona using the Grotrian's method.
Equipment: Telelens D/f = 200/1000 mm with the grating spectrograph
Spectrum of the scatterd light in the atmosphere
Target: Spectrum of the scattered light of the terrestrial atmosphere at a distance of 30 degrees from the Sun. This frame will be taken immediately after the second contact with a dispersion of 3 nm/mm in the spectral region of H-alpha. This picture will be taken with a grating spectrograph without of a lens. Analysis wil be used to check whether an emission of chromospheric lines very high in the solar corona is real, or it is a scattering in the terrestrial atmosphere.
Participants: M. Rybansky (head), L. Scheirich
Location: Balaton lake, Tihany, 46 degrees, 54 arcmin N, 17 degrees and 54 arcmin E, Hungary
Tatranska Lomnica, May 10, 1999
V. Rusin (vrusin@ta3.sk) and M. Rybansky (rybansky@ta3.sk)