The first device designed and manufactured at the Crimean Astrophysical Observatory (CrAO) for space observations was a solar short-wave diffraction spectrometer KDS, which worked on the third Soviet spaceship launched in 1959. Using this spectrometer equipped with an independent orientation control system, solar spectra in the wavelength region 304 Ê were registered [Bruns A.V., Prokof'ev V.K., 1961, Iskustvennie Sputniki Zemli, v.11]. The study of the Sun in far ultraviolet region was continued in 1967 on "Cosmos-166" satellite. As a result of this mission the variability of ultraviolet radiation during solar flares was discovered [Bruns A.V., Prokofiev V.K., Severny A.B., 1969, Ultraviolet observations: IAU Symp. N36, P. 187-180].

Further, sky background radiation became a subject of research. The special affords were directed to the evaluation of the physical properties of interplanetary and interstellar dust and gas from ultraviolet sky background observations. Using artificial satellites "Cosmos-51" (1964) and "Cosmos-213" (1968) having low-altitude orbits, the first experience in extra-atmospheric photometry of sky background was obtained. With a wide-angle (250 square degrees) two-channel photometer the radiation fluxes from broad sky areas were measured simultaneously in ultraviolet (2700 Ê) and visible (5400 Ê) spectral regions. A task of these experiments was to evaluate maximal and minimal values of sky radiation and to compare them with expected ones, calculated on the basis of the stellar atmosphere models, stellar statistics and zodiacal light data. Results of the experiments have shown, that the observed sky brightness on the Milky Way direction as well as on the Galactic Pole direction coincides with expected one within the accuracy of measurements [Dimov N.A., Zvereva A.M., Severny A.B., 1972, Izvestiya Krimskoy Astrophys. Observatorii, v.45, P.53-89].

These researches were followed by the experiment accomplished with the "Lunohod-2" lunar mission (1972) using an enhanced two-channel photometer: on January 16, 1973 for the first time the ultraviolet and visible brightness of the lunar sky was measured at the region of Lemonie crater. A careful preparation of the measuring equipment was required for the successful realisation of the experiment, taking into account fast and high temperature variability during the measurements. In close co-operation with the mission control team, manoeuvring with "Lunohod" and its cover, 12 successful observational sessions were accomplished during lunar day, twilight and lunar night. Brightness excess was registered in ultraviolet channel of the photometer (2700 Ê) and it exceeded expected one by 3-16 times. This fact evidenced the existence of a non-stationary lunar dust atmosphere with the optical thickness of 4¸10^-6. For two characteristic sizes of lunar soil grains equal to 10 and 70 mkm such optical thickness could be caused by 5 and 0.1 grains respectively in a column with 1cm² basis, and such low dust concentration above the lunar surface cannot be revealed during observations of the lunar edge from the Earth [Zvereva A.M., Severny A.B., Terez E.I., 1974, Kosmich. Issledovaniya v.12, N6, P.910-916; Zvereva A.M., Severniy A.B., Terez E.I., 1975, Izvestiya Krimskoy Astrophys. Observatorii, v.53, P.3-28.].

In 1974 measurements of resonance scattering in solar corona were done with an ultraviolet spectrometer on the satellite "Intercosmos-16". This device was developed and manufactured together with Swedish scientists, and it was the first experience of Crimean Observatory on cosmic project in international co-operation. [Bruns A.V., Stenflo J.O., Dravins D., Wihlborg N., Prokof'ev V.K., I.A.Zhitnik I.A., Biverot H., Solar Physics, 1980. vol 66.]

In 1975 ultraviolet spectra of the quiet sun and solar flares were obtained on the manned space station "Salut-4" with an orbital solar telescope "OST-1" designed and manufactured at CrAO. The specially constructed original stigmatic two-grating spectrograph permitted to receive UV-spectra of the Sun with a low level of the scattered light. The technological experiment of a drawing of reflecting covers on a mirror in the space directly was carried out for the first time in the world. The subsequent observation has shown good quality of the covers. The telescope had an autonomous (independent of the station) precise (2") orientation system. Astronauts, who have passed their practical training at CrAO, carried out astrophysical observations. Ground-based observations were organised in CrAO simultaneously with the space observations, which were performed out on-line with the Flight Control Center in Evpatoria. The processing of all obtained data was done at CrAO. As a result of this experiment more than 600 ultraviolet spectra of solar surface features and about 2000 images of the Sun were obtained, and more than 100 spectral lines in the wavelength region 900-1500 Ê were identified [Bruns A.V., Sidorov G.G., Steshenko N.V., 1979: Izvestiya Krimskoy Astrophys. Observatorii, v.59, P.57-63; Bruns A.V., 1979: Izvestiya Krimskoy Astrophys. Observatorii, v.59, P. 31-56; Bruns A.V., Grechko G.M.,Gubarev A.A., Klimuk P.I, Sevastyanov V.I., Steshenko N.V., Severny A.B., 1976, I.A.U. Colloquium N36: Energy balance and hydrodynamics of the Solar chromosphere and corona, Nice, France, Sept.1976, pp 333-372; Bruns A.V., Grechko G.M., Gubarev A.A., 1976, Space Research, Verlag - Berlin, v.16,pp.813-818. Bruns A.V., Grechko G.M.,Gubarev A.A., Klimuk P.I, Sevastyanov V.I., Severny A.B., Steshenko N.V., 1977, Space Research, Pergamon Press, Oxford and New York,vol.17,pp.509-513].

On high-apogee stations "Prognoz 6" (1977) and "Prognoz 7" (1978) - they were at the distance of 200,000 km from the Earth in their apogee - the ultraviolet spectrometer "GALAKTIKA" with field of view 36 square degrees was mounted. This device was developed at CrAO together with the Marceilles Laboratory of Space Researches. As a result of the experiment more than 4000 spectra of sky background were obtained in spectral region 1200-1900 Ê for 26 selected areas of the sky. Data from these stations are received in the Flight Control Centre in Evpatoria both in a mode of direct readout and in a mode of write-in. Large amount of data and new techniques of data processing allowed obtaining ultraviolet spectra of diffuse Galactic light in different sky directions both in low and high galactic latitudes. Analysis of the spectra has shown that in galactic latitudes less than 30 degrees the ultraviolet background agrees well with the models of diffuse galactic light; in galactic latitudes more than 30 degrees ultraviolet excess is observed. As a result it was found that this UV excess is connected with the emission from hot and dense features of gaseous hydrogen, which are sources of X-Ray sky background as well. [Zvereva A.M., Severny A.B., Granitzky L.V. at al. , 1982, Astron. and Astrophys.v. 116, P.312-322; Severny A.B., Zvereva A.M., 1983, Astrophys. Lett. v.23, P.71-77].

The first extra-atmospheric helioseismology experiment IFIR was accomplished by CrAO together with French and Swiss scientists on the interplanetary mission FOBOS. A device-precision photometer - worked while the spacecraft travelled to Mars. This experiment was unique because fluctuations of the solar radiation, being equal to one-millionth part of its average level, were measured practically continuously during 180 hours, at far distance from the Earth allowed to ignore terrestrial noises. Obtained data permit to evaluate parameters of global solar oscillations with the best accuracy reached so far and to discover pulsing variations of oscillation parameters with time [Bruns A.B., Bonne R., Delyabudiner J.P. et al. 1990, Pis'ma v astronomicheskiy Journal,v.16, N4, C.330; Bruns A.V., Shumko S.M., 1992, Izvestiya Krimskoy Astrophys. Observatorii, v.85, C.20]. The continuation of the solar oscillation studies at CrAO on more high experimental level was included in the research programme of the "MARS-96" mission (SOYA experiment). The device was constructed and manufactured, but the start of a space apparatus has passed unsuccessfully in 1996.

In 1983-1989 the largest Soviet ultraviolet mission was accomplished: space observations were carried out with astrophysical station "ASTRON", equipped with the 80-cm ultraviolet telescope. When "ASTRON " was launched, american mission "COPERNICUS" was the only space telescope with so large mirror. "ASTRON" was the first ultraviolet telescope launched into a high orbit, which gone away far beyond the limits of the Earth's magnetosphere. This is why the noises were minimised, and extremely faint objects were observed. The collaborators from the Marseilles Laboratory of Space Researches took direct part in the development of the scanning spectrometer with a concave grating mounted on the telescope. The X-Ray counters manufactured by collaborators from the Institute of Space Researches of the Russian Academy of Sciences were installed on the station "ASTRON" also. Collaborators from CrAO participated actively in every stage of this project: in the development of its scientific purposes and programme; in the design, manufacturing and testing of the telescope optics; in the design and manufacturing of the scanning spectrometer; in the assembly and alignment of a telescope in total; in the communication sessions with "ASTRON" in Deep Space Communication Centre in Eupatoria; in the processing and analysis of obtained data. Recently the monograph "Astrophysical Observations with the Space Station "ASTRON" was published [Boyarchuk A.A., Astrophysicheskie issledovaniya na kosmicheskoy stantzii ASTRON, M: Nauka, 1994, 419 pp], in which the whole material obtained in this experiment was gathered. Researchers from our country have acquired the most of their experience of astrophysical observations in Space with "ASTRON": numerous observations of the energy distributions in stellar spectra were carried out with this instrument; profiles of spectral lines evidencing the powerful flows of the stellar matter were recorded; sizes of hot components, invisible from the Earth, were estimated in dwarf double systems, where optical and X-Ray flares occur; intensities of many emission lines in extragalactic systems and in the spectra of diffuse nebulae in our Galaxy were evaluated; ultraviolet flares on a red dwarf star were registered with a record high time resolution; the rate of evaporation of Halley's Comet was estimated using molecular spectral bands observations; from changes in the spectrum of Supernova 1987 in Large Magellan Cloud the presence of thermonuclear fusion products was registered essentially earlier, than in other observations.

As a result of this mission the significant experience have been gained at CrAO in space observations in real time and in automated mode of the space telescope control: all observations on "ASTRON" was being made in real time, and telescope control is carried out at Deep Space Communication Centre in Eupatoria with the participation of astronomers from CrAO. All scientific information concerning ultraviolet observations was promptly processed in CrAO during one day, which allowed correcting quickly further observational programme. The final processing and analysis of all observational data was fulfilled in CrAO completely. Consideration of the results, obtained on "ASTRON", has shown that mirror coating of large-sized optics, made in CrAO optical workshop, suffered no degradation for the whole 6-year telescope lifetime.