Decayless low-amplitude transverse oscillations in short coronal loops as manifestations of dri v en slo w modes

A recent theoretical study of slow magnetoacoustic oscillations in a curved magnetic slab shows that the principal slow mode causes both dominant longitudinal motions and radial (transverse) kink-like motions of a slab. This modification of wave properties occurs due to the violation of the symmetry of wave motions with respect to the wav e guide axis and the slow to fast wave interaction in curved magnetic configurations. In this work, we carry out a comprehensive investigation of the principal slow mode depending on the model parameters. It is shown that the dominance of longitudinal motions in the principal slow mode decreases as both the internal plasma- βand slab aspect ratio increase. The results are used to explain the observed small amplitude decayless transverse oscillations in short coronal loops. In particular, these phenomena are interpreted as direct manifestation of slow mode oscillations in curved coronal loops excited at the footpoints by compressible oscillations of the underlying atmospheric layers. Numerical calculations have shown that the observ ed v elocity range of V = 0.6-5 km s -1 corresponds to radial velocity amplitudes in the principal slow mode, provided that the plasma- βinside the short loops is in the range of βi = 0.3-0.5 and the loop aspect ratio 0.15 ≤a/R ≤0.25. These parameters appear to be typical for low-lying small coronal loops extending from the transition region to the lower corona.