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We investigate the formation of discs within binary systems where at leastone component has left the main sequence. In particular we calculate theoccurrence rates of systems which can host long-lived, massive discs that maybe able to support the formation of planets. We synthesize a population basedon Milky Way properties, using both theoretical and observational inputs toconstrain key properties such as the shape of the initial mass function, binaryfraction, and mass transfer physics. We predict 0.26\% of binary systems willhost Second generation discs (where the primary has evolved), and 0.13\% ofsystems will host Third generation discs (where the secondary also evolves).For the Milky Way, this translates into 130 million and 90 million Second andThird generation systems respectively from an estimated total of 50 billionbinary systems. Of these systems that form discs, we estimate approximately20\% of Second and 3.8\% of Third generation discs have enough mass to form aplanetary system. We speculate on how the process of planet formation differsin these systems from conventional planet formation in protostellar discs.

The galactic rate of second and third generation disc and planet formation