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We find that $\sim 15-20$ per cent of A-type stars or red giants are boundwith a massive companion ($M_{\rm secondary} > 1M_{\odot}$) in an intermediatewide orbit ($0.5<P<5000\mbox{ yr}$). These massive binaries are expected toform wide-orbit, double-degenerate systems (WODDs) within $\lesssim10\mbox{Gyr}$ implying that $\sim10$ per cent of white dwarfs (WDs) are expected to bepart of a WODD with a lighter WD companion. These findings are based on ananalysis of previous adaptive optics observations of A-type stars and radialvelocity measurements of red giants and shed light on the claimed discrepancybetween the seemingly high multiplicity function of stars and the rather lownumber of detected double degenerates. We expect that GAIA will find $\sim 10$new WODDs within $20\mbox{ pc}$ from the sun. These results put a stringentconstraint on the collision model of type Ia supernovae in which triple stellarsystems that include a WODD as the inner binary are required to be abundant.

The Way To a Double Degenerate: $\sim15-20$ per cent of $1M_{\odot} \le M \le 8M_{\odot}$ Stars have a $M>1M_{\odot}$ Companion