  We have recently presented observational evidence which suggests that the
origin of the second generation (G2) stars in globular clusters (GCs) is due to
the binary-mediated collision of primordial (G1) low-mass main-sequence (MS)
stars. This mechanism avoids both the mass budget problem and the need of
external gas for dilution. Here, we report on another piece of evidence
supporting this scenario: (1) the fraction of MS binaries is proportional to
the fraction of G1 stars in GCs and, at the same time, (2) the smaller the
fraction of G1 stars is, the more deficient binaries of higher mass ratio
(q$>0.7$) are. They are, on average, harder than their smaller mass-ratio
counterparts due to higher binding energy at a given primary mass. Then (2)
implies that (1) is due to the merging\slash collisions of hard binaries rather
than to their disruption. These new results complemented by the present-day
data on binaries lead to the following conclusions: (i) the mass-ratio
distribution of binaries, particularly short-period ones, with low-mass
primaries, $M_{\rm P} < 1.5$ M$_{\sun}$, is strongly peaked close to q$=1.0$,
whereas (ii) dynamical processes at high stellar density tend to destroy softer
binaries and make hard (nearly) twin binaries to become even harder and favor
their mergers and collisions. G2 stars formed this way gain mass that virtually
doubles the primary one, $2M_{\rm P}$, at which the number of G1 stars is
$\sim5$ times smaller than at $M_{\rm P}$ according to the slope of a Milky
Way-like IMF at $M_{\rm MS} < 1.0$ M$_{\sun}$.
