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Various bright structures abound in the chromosphere playing an essentialrole in the dynamics and evolution therein. Tentatively identifying the wavecharacteristics in the outer solar atmosphere helps to understand this layerbetter. One of the most significant aspects of these characteristics is thewave phase speed (PS), which is a dominant contribution to solar coronalheating and Energy distribution in the Sun's atmosphere layers. To obtainenergy flux (EF), it is necessary to calculate the filling factor (FF) and thePS. In this study, the FF was determined by tracking the size and intensity ofthe IRIS bright points (BPs). To estimate an accurate PS and EF, it isnecessary to know the chromosphere and transition region (TR) thickness and thephase difference between the two desired levels. chromosphere and TR thicknesscannot be measured directly on the disc; This study is performed using spectraldata and calibrated based on Doppler velocities. As a result, the PSs in AR andCH, as well as for IRIS BPs have been calculated using the cross-power wavelettransform of Doppler velocities. Consequently, about CH, the PS mean values arefrom 40 to 180 km/s at network and from 30 to 140 km/s at internetwork; Andabout AR, are from 80 to 540 km/s at network and 70 to 220 km/s atinternetwork. Finally, the EF for the IRIS BPs has been calculated in threedifferent frequencies. The results indicate that the network BPs have aninfluential role in heating the higher layers while in the internetwork BPs,most of the energy returns to the lower layers.

A new approach to kinetic energy flux at the different frequencies above the IRIS Bright Points