Problems in Observation and Identification of Torsional Waves in the Lower Solar Atmosphere

The registration of periodic variations spectral line widths serves as the main method for observing torsional Alfvén waves. Theoretically, seems valid, yet it entails a number caveats when applied to data. For instance, amplitudes these observations should vary with changes location on disk and they be associated no intensity oscillations. We analyze extensive observational material non-thermal in coronal holes facular regions lines: H\(\alpha\), He i 10830 Å, Ca ii 8542 Ba 4554 Å. In most cases, we detected oscillations at similar frequencies. Besides, observed centre-to-limb dependency. This calls discussion practical validity alternative explanations nature widths. Based our observations, consider registering profile broadening necessary, but not sufficient, means unambiguous identification waves lower solar atmosphere.