Van den Heuvel et al. (1992) argued that the emission from supersoft X-ray sources can be explained by steady nuclear burning of hydrogen accreted onto massive white dwarfs. An argument that has been used against this model is that the bolometric luminosities inferred from blackbody fits are sometimes above the Eddington luminosity of a ∼1 M⊙ star. However, hot white dwarfs don't radiate blackbody spectra (Heise et al. 1994). Therefore, we have calculated model spectra for hot (accreting) white dwarfs, and investigated whether the emission from supersoft X-ray sources is consistent with an origin from white dwarfs. Here we summarize some preliminary results. For a review of supersoft X-ray sources we refer to the contribution of Kahabka & Trümper to these proceedings.