  The source G2 has already completed its pericentre passage around Sgr A*, the
super-massive black hole in the centre of our Galaxy. Although it has been
monitored for 15 years, its astrophysical nature and origin still remain
unknown. In this work, we aim to test the hypothesis of G2 being the result of
a stellar wind collision. To do so, we study the motion and final fate of gas
clumps formed as a result of collisions of stellar winds in massive binaries.
Our approach is based on a test-particle model in order to describe the
trajectories of such clumps. The model takes into account the gravitational
field of Sgr A*, the interaction of the clumps with the interstellar medium as
well as their finite lifetimes. Our analysis allows us to reject the hypothesis
based on four arguments: i) if G2 has followed a purely Keplerian orbit since
its formation, it cannot have been produced in any of the known massive
binaries since their motions are not consistent; ii) in general, gas clumps are
evaporated through thermal conduction on very short timescale (< 100yr) before
getting close enough to Sgr A*; iii) IRS 16SW, the best candidate for the
origin of G2, cannot generate clumps as massive as G2; and iv) clumps ejected
from IRS 16SW describe trajectories significantly different to the observed
motion of G2.
