We have discovered that the detached double degenerate binary WD 0957-666 has an orbital period of 1.46 hours, rather than the 1.15 day orbital period reported earlier. This is the shortest period example of such a system yet discovered. We obtain a unique period, which fits both our and earlier data. At this period the emission of gravitational radiation will cause the binary to merge within approximately 2.0 x 10*8 years. This system represents a population of short orbital period binaries which will merge within a Hubble time, and so could account for type Ia supernovae, although due to the low mass of both stars (0.3 to 0.4 solar masses), it is unlikely to become a supernova itself. We have detected the companion star and have measured a mass ratio of q = 1.15. This is the third double degenerate for which q has been measured and all three have q close to 1, which is in conflict with the predicted mass ratio distribution which peaks at 0.7. This system is viewed close to edge on, and we estimate that the probability of this system undergoing eclipses is 15 %.
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