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 can not 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 ( < 100 yr ) before getting close enough to Sgr A* ; iii ) IRS 16SW , the best candidate for the origin of G2 , can not generate clumps as massive as G2 ; and iv ) clumps ejected from IRS 16SW describe trajectories significantly different to the observed motion of G2 .