Coronal funnels, which originates from the networks at the photosphere, have great importance in terms of the mass up flows from lower to upper solar atmosphere. We have studied a North Polar Coronal Hole (NPCH) observation, which was observed on 10 October 2007 by Extreme Ultraviolet Imaging Spectrometer
(EIS) onboard Hinode, to identify the coronal funnels in the observed region. By the Gaussian fitting technique, we have estimated three basis parameters (e.g., Doppler velocity, FWHM, Intensity) on each location of the observed region. Extra FWHM locations (i.e., above a threshold level) have been identified in
quiet sun (QS), quiet sun with coronal hole boundary (QSCH) and coronal hole (CH) regions. For the density measurement, we have used the intensity ratio of
two density sensitive Fe XII lines and CHIANTI atomic data. On the basis of the variations of the parameters (e.g.,intensity,Doppler velocity,density), we have
shown that the excess width regions in the quiet sun are the coronal funnels. In the QSCH and CH regions, we have not found the favorable results to say that
the excess width locations in these regions are the coronal funnels. We have also found that plasma up flow starts at log 6.0 K and log 5.8 K in the quiet sun
and coronal holes respectively. Study of the temperature dependent behaviour of the nonthermal velocity is a forefront research in the solar physics now-a-days. In present analysis, nonthermal velocity decreases from Transition Region (TR) up to corona in the coronal hole as well as quiet sun. With the help of some previous results of nonthermal velocities, we have found that nonthermal velocity increase with temperature but after a certain temperature it decrease further. We have shown that Alfven wave propagation and dissipation as well as the prevalent occurrence of nano-flares at O VI formation temperature are two most probable responsible mechanisms for the explanation of nonthermal velocity.