### Observations of Dissipation of Slow Magneto-acoustic Waves in Polar Coronal Hole

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We focus on polar coronal hole region to find any evidence of dissipation of propagating slow magneto-acoustic waves. We obtained time-distance and frequency-distance maps along plume structure in polar coronal hole. We also obtained Fourier power maps of polar coronal hole in different frequency ranges in 171 \AA\ and 193 \AA\ passbands. We performed intensity distribution statistics in time domain at several locations in polar coronal hole. We find presence of propagating slow magneto-acoustic waves having temperature dependent propagation speeds. The wavelet analysis and Fourier power maps of polar coronal hole show that low-frequency waves are travelling longer distances (longer detection length) as compared to high-frequency waves. We found two distinct dissipation length scales of wave amplitude decay at two different height ranges (between 0-10 Mm and 10-70 Mm) along the observed plume structure. Dissipation length obtained at higher height range show some frequency dependence. Individual Fourier power spectrum at several locations show power-law distribution with frequency whereas probability density function (PDF) of intensity fluctuations in time show nearly Gaussian distributions. Propagating slow magneto-acoustic waves are getting heavily damped (small dissipation length) within the first 10 Mm distance. Beyond that waves are getting damped slowly with height. Frequency dependent dissipation length of wave propagation at higher heights may indicate possibility of wave dissipation due to thermal conduction, however, contribution from other dissipative parameters can not be ruled out. Power-law distributed power spectra were also found at lower heights in the solar corona which may provide a viable information on generation of longer period waves in the solar atmosphere.