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We present high precision, model independent, mass and radius measurementsfor 16 white dwarfs in detached eclipsing binaries and combine these withpreviously published data to test the theoretical white dwarf mass-radiusrelationship. We reach a mean precision of 2.4 per cent in mass and 2.7 percent in radius, with our best measurements reaching a precision of 0.3 per centin mass and 0.5 per cent in radius. We find excellent agreement between themeasured and predicted radii across a wide range of masses and temperatures. Wealso find the radii of all white dwarfs with masses less than 0.48M$_\odot$ tobe fully consistent with helium core models, but they are on average 9 per centlarger than those of carbon-oxygen core models. In contrast, white dwarfs withmasses larger than 0.52M$_\odot$ all have radii consistent with carbon-oxygencore models. Moreover, we find that all but one of the white dwarfs in oursample have radii consistent with possessing thick surface hydrogen envelopes($10^{-5} \ge M_\mathrm{H}/M_\mathrm{WD} \ge 10^{-4}$), implying that thesurface hydrogen layers of these white dwarfs are not obviously affected bycommon envelope evolution.

Testing the white dwarf mass-radius relationship with eclipsing binaries