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Recent observations with the Atmospheric Imaging Assembly (AIA) instrument onthe SDO spacecraft have revealed the existence of decayless coronal kinkoscillations. These transverse oscillations are not connected to any externalphenomena like flares or coronal mass ejections, and show significantly loweramplitudes than the externally excited decaying oscillations. Numerical studieshave managed to reproduce such decayless oscillations in the form of footpointdriven standing waves in coronal loops, and to treat them as a possiblemechanism for wave heating of the solar corona. Our aim is to investigate thecorrelation between the observed amplitudes of the oscillations and input theenergy flux from different drivers. We perform 3D MHD simulations in single,straight, density-enhanced coronal flux tubes for different drivers, in thepresence of gravity. Synthetic images at different spectral lines areconstructed with the use of the FoMo code. The development of theKelvin-Helmholtz instability leads to mixing of plasma between the flux tubeand the hot corona. Once the KHI is fully developed, the amplitudes of thedecayless oscillations show only a weak correlation with the driver strength.We find that low amplitude decayless kink oscillations may correspond tosignificant energy fluxes of the order of the radiative losses for the QuietSun. A clear correlation between the input energy flux and the observedamplitudes from our synthetic imaging data cannot be established. Strongerdrivers lead to higher vales of the line width estimated energy fluxes.Finally, estimations of the energy fluxes by spectroscopic data are affected bythe LOS angle, favoring combined analysis of imaging and spectroscopic data forsingle oscillating loops.

Amplitudes and energy fluxes of simulated decayless kink oscillations