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We present hydrodynamic simulations of gas clouds in the central kpc regionof the Milky Way that is modeled with a three-dimensional bar potential. Oursimulations consider realistic gas cooling and heating, star formation, andsupernova feedback. A ring of dense gas clouds forms as a result of X1-X2 orbittransfer, and our potential model results in a ring radius of ~200 pc, whichcoincides with the extraordinary reservoir of dense molecular clouds in theinner bulge, the Central Molecular Zone (CMZ). The gas clouds accumulated inthe CMZ can reach high enough densities to form stars, and with an appropriatechoice of simulation parameters, we successfully reproduce the observed gasmass and the star formation rate (SFR) in the CMZ, ~2x10^7 Msun and ~0.1Msun/yr. Star formation in our simulations takes place mostly in the outermostX2 orbits, and the SFR per unit surface area outside the CMZ is much lower.These facts suggest that the inner Galactic bulge may harbor a mild version ofthe nuclear star-forming rings seen in some external disk galaxies.Furthermore, from the relatively small size of the Milky Way's nuclear bulge,which is thought to be a result of sustained star formation in the CMZ, weinfer that the Galactic inner bulge probably had a shallower density profile orstronger bar elongation in the past.

Nuclear Star-Forming Ring of the Milky Way: Simulations