The solar corona has been the subject of intensive studies for several decades, serving as both the birthplace of space weather and a natural plasma physics laboratory. Kink oscillations of coronal loops are of particular interest due to their potential role in coronal heating and their application in plasma diagnostics. Two distinct regimes of kink oscillations have been detected: large-amplitude decaying kink oscillations, typically triggered by impulsive solar eruptions, and low-amplitude decayless kink oscillations, which are ubiquitous. The undamped nature of decayless oscillations suggests the presence of continuous energy input counteracts dissipation, though the exact physical mechanism remains debated. This talk focuses mainly on the observational properties and underlying mechanisms of decayless kink oscillations using data from the Atmospheric Imaging Assembly on the Solar Dynamics Observatory and the High Resolution Imager on the Solar Orbiter. Finally, I will discuss the dissipation of decayless oscillations and the recently observed high-frequency branch of this phenomenon.