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In this chapter we consider two formation channels for blue straggler stars:1) the merger of two single stars via a collision, and 2) those produced viamass transfer within a binary. We review how computer simulations show thatstellar collisions are likely to lead to relatively little mass loss and arethus effective in producing a young population of more-massive stars. Thenumber of blue straggler stars produced by collisions will tend to increasewith cluster mass. We review how the current population of blue straggler starsproduced from primordial binaries decreases with increasing cluster mass. Thisis because exchange encounters with third, single stars in the most massiveclusters tend to reduce the fraction of binaries containing a primary close tothe current turn-off mass. Rather, their primaries tend to be somewhat moremassive and have evolved off the main sequence, filling their Roche lobes inthe past, often converting their secondaries into blue straggler stars (butmore than 1 Gyr or so ago and thus they are no longer visible today as bluestraggler stars).

Formation Channels for Blue Straggler Stars