Mass ratios of double degenerate binaries

We have determined the orbital parameters and mass ratios of two newly identified double-lined double degenerate binary stars (WD 0136+768 and WD 1204+450) and improved these values for a third such system (WD 0957-666). Multiple Gaussian fitting to the double lined Her spectra was used to measure accurate orbital parameters for both the primary and secondary stars. For all three systems the mass ratio (q=M-1/M-2) was found to be close to, or in excess of, one. These values are in conflict with published theoretical distributions which peak at 0.5 to 0.7. We conclude that the evolution of double degenerates via an Algol-like phase, which allows for values of q close to one, needs to be included in theoretical mass ratio distribution models and that such an evolutionary channel is more important for the evolution of double degenerates than previously believed.