-Approved For Release4901/03126 : CIA-RDP96-00787ROO0500130064-s VMV 1.1,Tedne sLay, _,Tune 30,, 1971 117h 7848/B ;TROM-I,TG THE SUNIS SECRETS 7@ Scientists,@bf -the @@1,4"an ILsti Geomagnotisra.4 IonosDheE 7 L_oP_aE_-a @t_ll P testing a model of a Solar raulo-teiescope, The full scale teluscope will be orectod on a field of nearly fifty hectares in the Bodar district near Lake Baikalo Our correspondent asked -the director of the institute, _- - --- ---_---_ - ----. = Q corresponding member of the SR Academy of- Lof Sciences, Vladimir S-tepano@ and @he head 0 the la- b- 6 r -aIt.or"". rinad) _y Smolkov give their comment,-, of this@- Q. What was the reason for building; this radio-telescope? A. The Directives of -the 24th Congress of the CPSU provided for scientific research in the fields of long-distance radio communioatio-ns. television and weather forecasting in the coming five-year plan period, The scientists will also continue their research into the fundamental problems of astrophysics, interplanetary spaceg solar physics -and intoractions between the sun and earth, At present the sun presents us with unsolved puzzles concerning its spots, chromosphere eruptions and accompanying phenomena, Durin(, these bursts of activity the sun emits Lin enormous amount of energy in the form of waves and corpuscular radiation. The former take 8.3 minutes to reach the Earth, the latter several days. They cause interruption of radio communicntions, severe distortion of the Earth's magnetic field, affoct the vionther and even the condition of human beings suffering from Cardio-vascular diseases, The le-vol of radiation in the vicinity of the Earth increases to such an extent that it becomes, dangerous for cosmic flights, In order to learn how to -forecast these eruptive solar processes and their geophysical consequences, it is necessary to have full knowledge of their mochanism and dynamics. Q. But there are many other solar laboratories in the world, A. True. In our institute we havc Several .optical telescopes r for different purposes, They enable us to studN the surface, or photosphere of the sun, others the lower layers of the sola2.1 atmosphereq the ohro[nosphere. Using a tolescope, with a device for creating an artificial oolnr eclipse, i.e. a solar coronagraph we can study the outer layers of the sun's atmosphere, its ooron a , However we see only that ptirt which is at right angles to the line of sight and not that which faces the Earth, The latter will be visible either a we4k earlier or a week later due 'to the rotation of the Sun. OrUcal oboer-,ration is greatly dependent on the weather and thorefc):oe the instruments at our disposal are unable to cover all the aspects of solar rosearch. it is impossible to study the structure, dynamics@ origin and mechanisms in active areas of the @ r ataUiAre where these eruptions occur without the -use of s A @.rove For b lease 2001/03/26 : C 1A.RD P96 -00787 R0005001 30064-5 Approved For Releasv&2001/03/26 CIA-RDP96-00787RO005001 30064@5 '01 e d.n L,,sc',t,a-y 2 tadio-astronomical methods. For this reason the radio tel-eiscope is an essential aid the scientists, The pleasmal in the solar atmosphere radiates a continuous spectrum of rridio-waves. However the density of the atmosphere falls the further it is from the surface of the Sun. For this reason the wavelength of the radiation changas from a few millime,tres -near the surfaco of the Sun to tens of metres in the outer corona, 11L,,:,,diation of grea-Ler aller wavelengths or s m, is absorbed by the Earth's atmosphere, In the active areas of the corona, the density and temperature of the plasma is much hi.gher and the intensity of the radiation is greatly increased, By turning their radio-telescope to different wavelengths the scientists can Pexa-mine" the solar atmosphere at -various heightso The solar radio-telescope built several years ago in Australia is designed for wavelengths in the metre range. Ours will operate in the centimetre range. Q. What is the radio telescope like? A. It is a ,-@ulti-elament, cruc.-LforLn radio interferometre with two rows of antennas, one directed east-west, the other north-south, It is sup- lied with complex electronic equipment. P In designing the telescope many difficult technical problems had to be solved, For this reason it is necessary to check several of the technical problems connected with its design experimentally This is why we built this model.. It is not a miniature model, it consits of a number of antennae of the same size as the future telescope. The model will be used -to check the solar tracking devices, reception of radiation, etc. A wave-guide several hundred metres long will be set up to check the tracking of the signals received from the antennae, The large dimensions of the interferometer will give it high resolution, in the ncighbourhood of 20 seconds of arc, Panoramic ins- 1 1 simultaneouoly in two pection of the Sun will be porformec directions, The telescope will give us such an enormous amouiit of information tl@at -1-t -will be impossible -to process it by hand, The scanning and processing of the data will be performed automa-, tically by a computer which will control -the telescopeg collect and process the received signals and build a radio iMiage of the Sun every few minutes, At the same time the operator at the control panel will be able' -to see this image on the screen of a televisdon receiver. The radio telescope will be able to re,-ister local sources of radiation whoso intensity is ten times that of the quiescent solar corona. It will also be able to register eruptions which have al-.I- :' intensity a hundred times that of adjacent sources, It will enable us to f6llow fast transient processes in active areas of the lower layers of the co-rona. This will be the first ins-,trument in the'wo:@ld having such characteristics and capnbi li -ties. Approved For Release 2001/03/26 : CIA-RDP96-00787ROO0500130064-5 Allproved For Rele'aw 2001*103/26,: CIA-RDP96-010;7qZwROO0500130064-5 Wednesda 7 12L@@n-e 3 Q. What will this' instrument give science in the final analysis?. A. The instrut-iient at 13odar will be used for observations only, The theoretical conclusions from these observations will be drawn in the r&dio-,astronomical laboratories of the ins'titute which are connected by tele-tYPO with the interferometer. in the laboratories scientists will. be able to correlate processes observed by -the as radio-tolescopc with the structure of active aVeW observed optically in other observatbries of tho in,'-';'titute. Jilinallyq irve will be able to c-,)nstruct a map depicting the distribution of the Sun's magnetic field in space. With its help, scientists will be able to forecast solar activity, determine -the conditions for the transmission of radio signals and the conditions in space, All. this is necessary for ensuring dependable short-wAve radio communications between the Earth and objects in space, between different points on the surface of the globe and the snfety of life in '9pacet ;@ P/@ // 2" -3 Correspo Ling memb6r of the USSR Academy of Sciences, Aipistolkors@c@ is intimately concerned with the design of the radio @_eles@_c_5_6 -.He is scientific 'Otor of the prcj@@qtl, In designing 'an c o this instrument we 'f'&Fc71;@e conLYef from the observatories and institutes of the USSR Ao,,:tdc)my of Sciences, from the Presidium of the Siberian section of the A.So. and from industrial institutes and organisations, Q.,IWhen will the radio-telescope be put in-to, operation? A. We propose to finish working out the design problems of thel model in the present year, said GiSmol-kov, As soon as this is done we will start constructing the, system in Bodar, The site has already been selected and all preliminary work has been done, (Pravdg, May 23rdq 197'.T'. in full.) Approved For Release 2001/03/26: CIA-RDP96-00787ROO0500130064-5