  We explore the possibility that the G2 gas cloud falling in towards \sgra is
the mass loss envelope of a young TTauri star. As the star plunges to smaller
radius at 1000 to 6000 \kms, a strong bow shock forms where the stellar wind is
impacted by the hot X-ray emitting gas in the vicinity of \sgra. For a stellar
mass loss rate of $4\times10^{-8}$ \msun per yr and wind velocity 100 \kms, the
bow shock will have an emission measure ($EM = n^2 vol$) at a distance
$\sim10^{16}$ cm, similar to that inferred from the IR emission lines. The
ionization of the dense bow shock gas is potentially provided by collisional
ionization at the shock front and cooling radiation (X-ray and UV) from the
post shock gas. The former would predict a constant line flux as a function of
distance from \sgra, while the latter will have increasing emission at lesser
distances. In this model, the star and its mass loss wind should survive
pericenter passage since the wind is likely launched at 0.2 AU and this is much
less than the Roche radius at pericenter ($\sim3$ AU for a stellar mass of
2\msun). In this model, the emission cloud will probably survive pericenter
passage, discriminating this scenario from others.
