Abstract. We present the first estimation of far ultraviolet (FUV: 1000 - 1150 \AA) diffuse radiation from the Small Magellanic Cloud (SMC) based on observations made with the {\em Far Ultraviolet Spectroscopic Explorer (FUSE)}. We have adopted the data analysis method of Murthy and Sahnow (2004) for extraction of diffuse surface brightnesses from the {\em FUSE} spectra. The diffuse radiation is primarily due to light from hot stars scattered by the interstellar dust grains. The FUV diffuse surface brightness in the SMC ranges from around 10³ photons cm^-2s^-1 sr^-1 A^-1 to as high as 2.5 × 10⁵ photons cm^-2 s^-1 sr^-1 A^-1. We have estimated the fraction of the total radiation in the field emitted as diffuse radiation which is about 40% - 50%. We found that much less light is scattered in the FUV than at longer wavelengths with the stellar radiation going into heating the interstellar dust. The FUV diffuse fraction from the SMC is much higher than the Large Magellanic Cloud (LMC: Pradhan et al. 2010) due to less number of young hot stars in the SMC compared to the LMC.