Weak Damping of Propagating MHD Kink Waves in the Quiescent Corona

Propagating transverse waves are thought to be a key transporter of Poynting flux throughout the Sun's atmosphere. Recent studies have shown that these motions, interpreted as magnetohydrodynamic kink mode, prevalent corona. The associated energy estimates suggest carry enough meet demands coronal radiative losses in quiescent Sun. However, it is still unclear how deposit their into plasma. We present results from large-scale study propagating corona using data Coronal Multi-channel Polarimeter (CoMP). analysis reveals appear weakly damped, which would imply low rates transfer motions smaller-scales via either uni-turbulence or resonant absorption. This raises questions about observed modes Moreover, observations, combined with Monte Carlo simulations, lead us infer solar displays spectrum density ratios, smaller ratio (relative ambient corona) loops and higher active region loops.