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We have presented an ab \ initio model of the 2 μ m spectral features of (H2)2 based on the far-infrared models of McKellar & Schaefer (1991). We have shown that the intensity variations of the 2 μ m (H2)2 features depend on the ortho/para ratios of H2. We have discussed the applicability of the variations to the atmospheres of the giant planets for the derivations of the ortho/para ratios. The signal to noise ratios of currently available spectra of the giant planets are not sufficient enough to derive accurate ortho/para ratios of these planets. Observations with longer exposure times and larger telescope apertures are required to obtain better spectra for the derivations of the ortho/para ratios of H2 in the atmospheres of the giant planets.