The origin of the dense gas cloud G2 discovered in the Galactic Center ( ) is still a debated puzzle .
G2 might be a diffuse cloud or the result of an outflow from an invisible star embedded in it .
We present hydrodynamical simulations of the evolution of different spherically symmetric winds of a stellar object embedded in G2 .
We find that the interaction with the ambient medium and with the extreme gravitational field of the supermassive black hole in the Galactic Center must be taken into account for such a source scenario .
The thermal pressure of the hot and dense atmosphere confines the wind , while its ram pressure shapes it via stripping along the orbit , with the details depending on the wind parameters .
Tidal forces squeeze the wind near pericenter , reducing it to a thin and elongated filament .
We also find that in this scenario most of the Br \gamma luminosity is expected to come from the densest part of the wind , which has a highly filamentary structure with low filling factor .
For our assumed atmosphere , the observations can be best matched by a mass outflow rate of \dot { M } \mathrm { { } _ { w } = 8.8 \times 10 ^ { -8 } M _ { \odot } yr ^ { -1 } } and a wind velocity of v \mathrm { { } _ { w } = 50 km / s } .
These values are compatible with those of a young T Tauri star wind , as already suggested by .