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We carry out a series of simulations of G2-type clouds interacting with theblack hole at the galactic center, to determine why no large changes in theluminosity of Sgr A* were seen, and to determine the nature of G2. We measurethe accretion rate from the gas cloud onto Sgr A* for a range of simulationparameters, such as cloud structure, background structure, background density,grid resolution, and accretion radius. For a broad range of parameters, theamount of cloud material accreted is small relative to the amount of backgroundmaterial accreted. The total accretion rate is not significantly effected forat least 30 years after periapsis. We find that reproducing observations of G2likely requires two components for the object: an extended, cold gas cloudresponsible for the Br-gamma emission, and a compact core or dusty stellarobject dominating the bolometric luminosity. In simulations, the bolometric andX-ray luminosity have a peak lasting from about 1 year before to 1 year afterperiapsis, a feature not detected in observations. Our simulated Br-gammaemission is largely consistent with observations leading up to periapsis, witha slight increase in luminosity and a large increase in the FWHM of the linevelocity. All emission from a gaseous component of G2 should fade rapidly afterperiapsis and be undetectable after 1 year, due to shock heating and expansionof the cloud. Any remaining emission should be from the compact component ofG2.

G2 and Sgr A*: A Cosmic Fizzle At The Galactic Center