Figure 1 - uploaded by A. A. Hady
Content may be subject to copyright.
Panel a shows equatorial electron density and Panel b shows average equatorial electron density vs 1/x in the equatorial plain of June 21, 2001 solar corona.

Panel a shows equatorial electron density and Panel b shows average equatorial electron density vs 1/x in the equatorial plain of June 21, 2001 solar corona.

Source publication
Article
Full-text available
Five series of coronal images have been obtained by V.Kulijanishvili during the total solar eclipse of the June 21, 2001, in Zambia, Lusaka. A photographic mirror-lens coronagraph-polarimeter (D=100 mm, F=1000 mm) was used. The absolute brightness, polarization and direction of polarization of the inner corona were measured. Standard techniques are...

Similar publications

Article
Full-text available
The good quality of the observing sequence of about 60 photographs of the white-light corona taken during the total solar eclipse observations on 29 March 2006, in Al Sallum, Egypt, enable us to use a new method of image processing for enhancement of the fine structure of coronal phenomena. We present selected magnetic-field lines derived for diffe...
Article
Full-text available
Results from photographic observations of the white light solar corona conducted during the total phase of the total solar eclipse on March 29, 2006 in Manavgat, Turkey are shown in this work. Spectroscopic study of the green 530.3nm line of Fe XIV in the corona of the Sun has also been made. The spectrograph was designed by specialists from the ST...
Article
Full-text available
White light corona observations during 3 total solar eclipses (1999, 2006 and 2009) at different phases of the solar cycle, and comparative analysis of the results are presented in this work.Photos are made with objectives with different focus and exposure. Structures of the coronas are determined from composite images. Solar corona flattening is d...
Article
Full-text available
In this work we measured light intensity as a function of time during a total solar eclipse using a solar cell. The measured intensity was corrected for the detector response and compared with a mathematical expression that represents the uncovered apparent area of the solar disk as a function of time. By no means, this corrected intensity is linea...
Article
Full-text available
We report on white light observations of high latitude tethered prominences acquired during the total solar eclipses of 2012 November 13 and 2013 November 3, at solar maximum, with a field of view spanning several solar radii. Distinguished by their pinkish hue, characteristic of emission from neutral hydrogen and helium, the four tethered prominen...

Citations

Article
Full-text available
The space science research has been started in Egypt since 1910 by measuring the solar constant as indication of solar radiation at Helwan Observatory. The solar sunspot studies and its influence on the Nile flooding was erected and operated at Helwan as a first solar station in Egypt during 1957. Zeiss-Coude’ refractor was installed in 1964. Astronomy and space science educations started in Egypt at the university level since 1936 at Department of Astronomy and Meteorology of Cairo University. Undergraduate and graduate education in Egypt will be discussed in this work.The total solar eclipse observations on 25th February, 1952 in Khartoum have been done by on Egyptian–French group by using the Worthington Camera. Several international groups observed the total solar eclipse on 29 March 2006, in El-Saloum (Egypt). A coordinated effort partly undertaken in the frame of the French–Egyptian scientific cooperation permitted joined simultaneous eclipse observations of the solar corona. Several Ground base instrumental set-up has been prepared. Spaceborne quasi-simultaneous EIT and Lasco observations of SoHO have been used as well as TRACE observations in Lyman-alpha of HI. W-L images taken with and without a radial filter are processed to show the magnetic structure of the corona. Polarization analysis is performed to study the F-corona in the outer corona. Several filters have been obtained to show the distribution of the emission measures of the inner and middle corona. Spectra were obtained over several emission lines.