Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21733548k&link_type=abstract
American Astronomical Society, AAS Meeting #217, #335.48; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
We present hydrodynamic simulations of gas clouds in the central kpc region of the Milky Way that is modeled with a three-dimensional bar potential. Our simulations consider realistic gas cooling and heating, star formation, and supernova feedback. As found in previous two-dimensional simulations, gas clouds undergo an abrupt loss of angular momentum at the cusps of the innermost closed, elongated orbits along the bar (X1 orbits), plunge to a new family of orbits much deeper in the potential (X2 orbits), and accumulate there forming the Central Molecular Zone (CMZ). We find that the gas clouds in the X2 orbits can reach high enough densities to form stars, and our star formation rates are consistent with observationally inferred SFR values, a fraction of 0.1 M&sun; yr-1, obtained by Yusef-Zadeh et al. Star formation in our simulations takes place mostly in the outermost X2 orbits with a radius of 200 pc, and this suggests that the star formation observed in the CMZ may be a mini version the of nuclear star forming ring seen in some external disk galaxies.
Figer Donald F.
Jeon Myoungwon
Kim Sungsoo S.
Merritt David
Saitoh Takayuki R.
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