315 



!frn = g;(f/f„,) (13) 



where \\i denotes a dimensionless qjuantity representing a "ur.iversal" 

 spectral density function. 



Typical smoothed spectra which have been smoothed and corrected for 

 noise level after Eidy and Plate (1965) are plotted in a form corresponding 

 to Eq. (12) in Figure 16. The spectra in Figure 16 serve to define the 

 similarity function ^ quite well. The conditions of Uqq, f and d for these 

 spectra are shown in Table III along with the values of cj , f and * . 

 In general, it was found that the channel data followed ^ quite satis- 

 factorily for the range 6 <U < 15 mps, and for 3 <F< 12 meters. 



According to Phillips (l958aj> on dimensional grounds, the equilibrium 

 or saturation region in the high frequency region of the spectra for gravity 

 waves should follow the f~^ rule. In contrast, it has been suggested by 

 Hicks (see, for example, Phillips ( 1958b)) that the pure capillary spectrum 

 should follow an f'l/S rule. As indicated in Figure 16, the dimensionless 

 spectra for waves in the chajanel tend to follow the f"^ rule over approxi- 

 mately two decades in the high frequency range. In the highest frequency 

 ratios, there is a tendency for some of the spectra to develop a slope less 

 than -5- Capillary wave behavior should begin to appear above f = 13 cps 

 in the frequency spectra. Only two cases, numbers 163 and I88 as shown in 

 Figure 16, actually reach this range. For case 163, capillary waves should 

 appear for f/fj^ = 2.7 to 3.O, while, for case I88, f/f^ = 6.8 to 7.0. Thus, 

 in Figure 16, these two examples may display the beginnings of a transition 

 to the f"T/3 range. 



