We detect the HD 32297 debris disk in scattered light at 1.6 and 2.05 µm .
We use these new observations together with a previous scattered light image of the disk at 1.1 µm to examine the structure and scattering efficiency of the disk as a function of wavelength .
In addition to surface brightness asymmetries and a warped morphology beyond \sim 1 \farcs 5 for one lobe of the disk , we find that there exists an asymmetry in the spectral features of the grains between the northeastern and southwestern lobes .
The mostly neutral color of the disk lobes imply roughly 1 µm-sized grains are responsible for the scattering .
We find that the asymmetries in color and morphology can plausibly be explained by HD 32297 ’ s motion into a dense ISM cloud at a relative velocity of 15 km s ^ { -1 } .
We model the interaction of dust grains with HI gas in the cloud .
We argue that supersonic ballistic drag can explain the morphology of the debris disks of HD 32297 , HD 15115 , and HD 61005 .