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The Siberian Solar Radio Telescope (SSRT) of the Institute of Solar-Terrestrial Physics is located at a short distance from Lake Baikal. A continuous monitoring of solar activity is being carried out during the daytime at this telescope.
The SSRT is a phased cross-shaped 128 x 128 antenna array. Until recently, the routine observation mode at the SSRT (wavelength = 5.2 cm; down to 15 arcsec angular resolution) was additive one-dimensional scanning of the solar disk with North-South and East-West baseline interferometers.
In late 1995, the two-dimensional mode observations started to produce full-disk images for a time interval as long as 3 minutes, and they have been providing images every day since the spring of 1996. Because of the present impossibility of ensuring long-term storage of all information obtained, only two or three solar disk images per day are stored.
Within the Sun-Earth Connection Collaborative Project of the Astronomy On-Line Programme, some of these images will be made available to the participants from this page.
Now we send the series of the SSRT images on October 31 and November 2, 4. The Sun is quiet now. This set of images is the last one within this phase of the Astronomy On-Line programme. Also we will have a short preventive break in the SSRT correlative mode operation. But we are ready to continue collaboration with you or with your colleagues. We could also send our images to some WWW-site place if such a possibility will exist in future.
We send the images of the solar disk on October 25,26,27,28,29,30. These maps are oriented heliocentrically, the north is at the top, the west is on the right.
We send here the images of the solar disk on October 20, 22, 23, 1996, which seem to be reasonably well and are quite interesting.
In the southern hemisphere, there are plages with a plage filament in the middle. Plage areas are well identified with non-compact areas of enhanced brightness in our maps. At our observational frequency, filaments are rather weak dark objects, and therefore are not always detectable. Nevertheless, the presence of the dark plage filament is appreciable on the maps of October 22 and 23. On October 20, the filament is seen poorly because of presence of rather bright loop covering the filament channel. In turn, in the northern hemisphere, it is possible to see a horizontal dark strip, which corresponds to a high-latitude filament. Some point sources of medium intensity on a solar disk are identified with bright X-ray points present on the YOHKOH images.
These maps are oriented heliocentrically, the north is at the top, the west is on the right.
On behalf of my colleagues, A. Uralov (SSRT).
Institute of Solar-Terrestrial Physics
(ISTP)
Siberian Division of RAS
p/b 4026
RUS-664033
Irkutsk
Russia
To obtain additional information about the SSRT two-dimensional operation mode and about the availability of solar disk radio images, please contact Dr. Arkadii Uralov by E-mail at uralov@sitmis.irkutsk.su.