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Cosmic Ray Nucleonic Intensity in Low-Amplitude Days During the Passage of High-Speed Solar Wind Streams One of the most striking features of solar wind is its organization into high- and low- speed streams. It is now well established that the passage over the Earth of high-speed solar wind streams leads to geomagnetic disturbances. The high-speed plasma streams are thus a key element in the complex chain of events that link geomagnetic activity to the solar activity and are therefore of great interest to the solar terrestrial physics. Two types of high-speed solar wind streams - coronal-hole-associated (or corotating) and flare-generated - were studied based on magnetic field and solar wind plasma parameters. In the work, the dependence was obtained for cosmic ray (CR) depressions due to high-speed solar wind streams during low-amplitude days. The CR nucleonic intensity data were subjected to the superposed epoch analysis with respect to the start time of high-speed solar wind streams. It was found that streams of both types produce significant deviations in the CR intensity during low-amplitude anisotropic wave train events. At the onset of such streams the CR intensity reaches its minimum during low-amplitude events and then increases statistically. Viena no Saules vēja pārsteidzošākajām īpatnībām ir tā, ka veidojas divu tipu plūsmas - liela un maza ātruma plūsmas. Noteikts, ka nonākot uz Zemes liela ātruma Saules vēja plūsmām, rodas Geomagnētiskās vētras. Ātri darbīgās plazmu plūsmas ir galvenie elementi, kas izsauc geomagnētisko darbību saistītu ar Saules darbību, un tāpēc ir liela interese par Zemes fiziku un Sauli. Šie ātrdarbīgās plūsmas divi tipi tiek klasificēti divās kategorijās, kuru pamatā ir magnētisko lauku un Saules vēja parametri. Mēs pētījām kosmiskā starojuma depresiju saistībā ar ātrdarbīgām Saules vēja plūsmām mazu amplitūdu dienās. Kosmisko staru intensitātes dati analizēti no Saules vēja ātri darbīgo plūsmu parādīšanās sākuma. Saules vēja divu tipu plūsmas rada būtisku novirzi kosmiskā starojuma intensitātē mazu amplitūdu laikā. Sākumā kosmiskā starojuma intensitāte sasniedz minimumu mazu amplitūdu dienās, bet pēc tam palielinās statistiski.