  Young massive stars in the central parsec of our Galaxy are best explained by
star formation within at least one, and possibly two, massive self-gravitating
gaseous discs. With help of numerical simulations, we here consider whether the
observed population of young stars could have originated from a large angle
collision of two massive gaseous clouds at R approx. 1 parsec from Sgr A*. In
all the simulations performed, the post-collision gas flow forms an inner,
nearly circular gaseous disc and one or two eccentric outer filaments,
consistent with the observations. Furthermore, the radial stellar mass
distribution is always very steep, Sigma proportional to R^-2, again consistent
with the observations. All of our simulations produce discs that are warped by
between 30 to 60 degrees, in accordance with the most recent observations. The
3D velocity structure of the stellar distribution is sensitive to initial
conditions (e.g., the impact parameter of the clouds) and gas cooling details.
For example, the runs in which the inner disc is fed intermittently with
material possessing fluctuating angular momentum result in multiple stellar
discs with different orbital orientations, contradicting the observed data. In
all the cases the amount of gas accreted by our inner boundary condition is
large, enough to allow Sgr A* to radiate near its Eddington limit over approx.
10^5 years. This suggests that a refined model would have physically larger
clouds (or a cloud and a disc such as the circumnuclear disc) colliding at a
distance of a few parsecs rather than 1 parsec as in our simulations.
