Comparison between the observed spectrum of U Gem (after the orbital motion has been removed) and the best‐fitting solar abundance WD model spectrum. The temperature of the model is 31,000 K and log g is 8.5. Although in a general sense the correct lines appear in the model spectrum with about the right line ratios, most of the lines in the model are stronger than what is observed in the U Gem spectrum. A very prominent exception to this general rule is the N III complex at 1184 Å, which is weaker in the model spectrum.