  Various bright structures abound in the chromosphere playing an essential
role in the dynamics and evolution therein. Tentatively identifying the wave
characteristics in the outer solar atmosphere helps to understand this layer
better. One of the most significant aspects of these characteristics is the
wave phase speed (PS), which is a dominant contribution to solar coronal
heating and Energy distribution in the Sun's atmosphere layers. To obtain
energy flux (EF), it is necessary to calculate the filling factor (FF) and the
PS. In this study, the FF was determined by tracking the size and intensity of
the IRIS bright points (BPs). To estimate an accurate PS and EF, it is
necessary to know the chromosphere and transition region (TR) thickness and the
phase difference between the two desired levels. chromosphere and TR thickness
cannot be measured directly on the disc; This study is performed using spectral
data and calibrated based on Doppler velocities. As a result, the PSs in AR and
CH, as well as for IRIS BPs have been calculated using the cross-power wavelet
transform of Doppler velocities. Consequently, about CH, the PS mean values are
from 40 to 180 km/s at network and from 30 to 140 km/s at internetwork; And
about AR, are from 80 to 540 km/s at network and 70 to 220 km/s at
internetwork. Finally, the EF for the IRIS BPs has been calculated in three
different frequencies. The results indicate that the network BPs have an
influential role in heating the higher layers while in the internetwork BPs,
most of the energy returns to the lower layers.
