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Decayless kink oscillations are omnipresent in the solar atmosphere and aviable candidate for coronal heating. Though there have been extensive studiesof decayless oscillations in coronal loops with a few hundred Mm lengths, theproperties of these oscillations in small-scale ($\sim$10 Mm) loops are yet tobe explored. In this study, we present the properties of decayless oscillationsin small loops embedded in the quiet corona and coronal holes. We use highresolution observations from the Extreme Ultraviolet Imager onboard SolarOrbiter with pixel scales of 210 km and 5 s cadence or better. We find 42oscillations in 33 coronal loops with loop lengths varying between 3 to 23 Mm.The average displacement amplitude is found to be 136 km. The oscillationsperiod has a range of 27 to 276 s, and the velocity amplitudes range from 2.2to 19.3 km s$^{-1}$. The observed kink speeds are lower than those observed inactive region coronal loops. The variation of loop length with the period doesnot indicate a strong correlation. Coronal seismology technique indicated anaverage magnetic field value of 2.1 G. We estimate the energy flux with a broadrange of 0.6-314 W m$^{-2}$. Moreover, we note that the short-period decaylessoscillations are not prevalent in the quiet Sun and coronal holes. Therefore,our study suggests that decayless oscillations in small-scale coronal loops areunlikely to provide enough energy to heat the quiet Sun and accelerate solarwind in the coronal holes.

A Statistical Investigation of Decayless Oscillations in Small-scale Coronal Loops Observed by Solar Orbiter/EUI