Special attention should be paid to oscillations detected in the upper solar atmosphere, as they may reflect the transport of energy into the corona by magnetohydrodynamic (MHD) waves. The aim of this study is to investigate the non-stationary physical processes taking place in solar spicules and prominences, as well as the relationship between them. The study and comparison of spicules and prominences, and the obtained results, will introduce certain new insights for explaining the physical processes occurring within them. At the Abastumani Astrophysical Observatory, spectrograms in the hydrogen H $\alpha $ line were obtained at two different heights (7500 km and 8000 km) with the aid of a large, non-eclipse coronagraph. The standard errors in the determination of Doppler velocities and FWHM are ±0.35 km/s and 0.04 Å, respectively. The lifetimes of almost all measured spicules were about 20 minutes, thus resembling type I spicules. Future observational and theoretical studies will contribute to a better understanding of the nature of phenomena occurring in the solar atmosphere and to clarifying possible links between them. From the processing and analysis of the observational material, the following results were obtained: (1) For H $\alpha$ prominences, no asymmetry was found in the temporal variations of Doppler velocities and half-widths. (2) In H $\alpha$ spicules and prominences, the time variation of Doppler velocities proceeds in approximately the same manner. (3) An asymmetry in the temporal variation of half-widths was detected in H $\alpha $ spicules and prominences. (4) In Sect. 1, a brief overview of the study of spicules and prominences is presented. (5) In Sect. 2, the observations and data processing are described. (6) In Sect. 3, the analysis of observational data, including Doppler velocities and FWHM, is discussed. (7) In Sect. 4, the discussion and conclusions are presented.
