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  1. 2020-05-04T14:01:32+00:00Z 281 SH 5 1-18 STUDY THE SCINTILLATOR NEYWORK OF COS},:IC RAY SCINTILLATIONS T_ESCOPE STATIONS FROM 5-MINUTE DATA OF "IZMIRAN" AND WORLD-WIDE O.V.Gulinsky, K.F.Yudakhin L.I.Dorman, I.Ya.Libin, R.E.Prilutsky, Institute Wave propagation, Moscow Region, USSR of Terrestrial }_agnetism_ Ionosphere USSR Academy of Sciences, and Radio I_2092 Troitsk During cosmic ray propagation there appear characteristic lations 7I/ which are due to charged particle on random inhomogeneities field (IMF). Particles sensitive not only to IMF inhomogeneities, fine structure of approaching gest scintillations. Nonetheless, than several Gev) cosmic ray scintillations, stered in the most sensitive way be ground-based used for recording cosmic radiation, tive. From the physical ed with the fact that a particle (R = C_/e#>_RC Rc is the correlation netic field) "sses" a wide spectrum whereas when interacting the magnetic inhomogeneity bring information about a comparatively the INF turbulence spectrum. The smallness of scintillation energy range is compensated in this energy range are made by ground-based a significant statistics The power spectra of cosmic ray scintillations Earth during some intervals from 1977 to I982 riods, for solar flares and Forbush shock waves, Fig. I) have been calculated one- and two-hour values red by the scintillator supertelescope tions of the world-wide network Apatity, Tixie Bay, Norikura). by the methods of spectral methods which mutually control possible not only to analyze guished frequencies, but also to determine spectrum slopes in some frequency I1 the power-law spectrum is described by the power the ratio of the soectrum values ranges f< 8 . IO-_Hz and IO-_ f_ IO-eHz tors and scintillator telescopes in interplanetary cosmic-ray intensity space scientil- scattering magretic which are but also to the undergo the lar- (more which are regi- devices are similarly of view this is also connect- with a large Larmor radius of a random mag- of IMF inhomogeneities, with the high-frequency spectrum, low-energy narrow region of of the interplanetary of rather low energies shock fronts, the high-energy informa- point radius part particles of amplitude in the high- by the fact that measurements devices with /2/. and a high accuracy on the (for quiet pe- due to power from five-minute, intensity measu- IZMIRAN and in sta- (Moscow, Utrecht, The spectra were estimated analysis and by autoregressive each other /3/ and make it scintillation powers the behavior ranges. of cosmic ray scintillations function P(f)NA in different frequency (for neutron moni- of the world-wide decreases of the cosmic-ray Kerguelen, at distin- of f-_, then using net of

  2. 282 SH 5 1-18 stations), tion that the IMF spectrum remains one can evaluate the product HoV (in the assump- unchanged in the entire frequency 3oo_.v'-- 2_ n-I ."+td _'" "1./ ''_<" .... JL £ is determined de as range) i ] The I_F scintillation spectrum -s v,, ,x .] m. n(fJ rsJ ,2 where locity, are coupling Mean scintillation stations Moscow, Baksan, for frequencies the interval IO-" the index lies wlthin for frequencies is due to the competition Ho is n the mean IMF strength, is the index of pitch-angular coefficients estimations of the indices of the slopes power spectra for different Utrecht, Kerguelen, Apatity in quiet _eriods f_3 _IO IHz the spectral I.@5 _ _ 1.75, 1.95 _ f >3 IO _ Hz 1.55 _ between V is the solar distribution, of the devices. wind ve- W(R) of CR in the devices Stir, Vostok, results: index _ @"I0-6__ _'_<3.35 and, finally, _'_ 2.I0 (the latter the GR scintillation Lomnicky give the following lies i_ for frequencies po- wer and the noise power P(f)/n_ of the power spectra _he :values of $ both with the results (the relation between the spectral _, has the form IO- and /= _ presents the power over the investigated maximum (cur_e I) and the minimum tivity. For all the frequencies the well with the theoretically 5-IO-S_s and v = 5*IO7 cm-s-_) both in the absolute (in the high-frequency range 1.5 and in the low-frequency and in the behaviour of the spectra: ces coincide with an accuracy There exist also other possibilities OR scintillation spectrum: wer spectrum of INLFfluctuations, to-one correspondence with the level of perturbation terplanetary medium of both distinguished certain frequencies and the spectrum of the OR scintillation spectrum creases gradually up to the maximum value fore the perturbation of interplanetary Earth. Figure 3 shows the behaviour = 2/no). The calculations ) of IMF fluctuations of 1.8+_O.I, which experiments and of ref./%/ indices of IN[F, Q and CR, _ = 9 + 2 in the frequency_ range _-IO for frequencles f _ 3 IO-_Hz). spectra for CR scintillations stations for different periods (curves 2,3) of solar ac- power calculated values ( _ /-$ give of the order of field agrees well g_,r_ 2 Figure averaged of the values coincide /@/ (for Ho= values of 1.2- they differ by a factor range by a factor the values to IO %. of 1.5-2) of the indi- for studying the one can not only estimate but also establish a one- the po- in in- scintillations as a whole - the slope in the range f_IO-_Hz several hours be- medium comes to the of the index of the po- at in-

  3. 283 SH 5.1-18 wet spectrum ber I977 from the data of the Utrecht and Kerguelen tions. It is seen from the figure that at least I8 hour@ beforejperturbation the soectral of CR scintillations for the events in Septem- sta- index in the range IO-_/_ _<IO-_Hz the spectrum CR go ahead inhomogeneities tering sand times larger than the velocity turbation. Hence, taneously, whereas perturbation hours. Therefore, aching the Earth particles of different neities at distances starts increasing is given in the form A /-6 of perturbation at a di@tance (about IO 'z- IO "_ cm) and their velocity whereas .the_ quantity A (if That feel ) decreases. can be easily explained:CR of their free path for scat- is a thou- of per- instan- of propagation practically travels to the Earth between perturbations different: energies, one can observe up to several AU. CR bring information long appro- the distances can be essentially recording inhomoge- REFERENCES I. L.I. Dorman., 9_-152. 2. L.I. method for cosmic ray scintillation I979. 3. O.V. Gulinsky., the Conference, 4. L.I. Dormane, _.E. Katz, _i. Steglik ser. fiz. I983, IoYa. Libin - Space Sci.Rev., I98_, 39, Dorman., I.Ya. Libin, Ya.L. Blokh - Scintillation studies - _., Nauka, L.I. Dorman., R.E. Prilutsky. Proc. of et al. - Izv. AN SSSR _7, Ng, I986. _0 Z0t5 PmZIO_ !Omirt t

  4. . - 3- 2 . fig. 2 frp. 3 FREQUENCY, SEPTEMBER, i n K i977 f3 . 1 4 . 1 5 , 1 6 . 1 7 , 18. 19 , 20, 21, 2 2 , 23 - P(f) 2 8 . f - * a 9 . fO . t! . 12 7 . 8 4,0 3,* . FD BE ! . . . BE' 1 0.4 FD . . . . . . . ........ ................ ........ .... ....... 6 .*.' 4 ' . : . .. • 1 BE- BEGlNING OF EFFECT Fa- ~ & U H urRECHT 4 IERCELEN b =RASE __-- L