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18-02-2010
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Today's colloquium: Star Formation in the Central Molecular Zone of the Milky Way (Sungsoo Kim, Kyung Hee University, Korea)

Submitter: Jean-Mathias Griessmeier
Description: Gas materials in the inner Galactic disk continuously migrates toward the Galactic center (GC) due to interactions with the bar potential, magnetic fields, stars, and other gaseous material. Those in forms of molecules appear to accumulate around 200 pc from the center to form stars there and further inside. The bar potential in the GC is thought to be responsible for such accumulation of molecules and subsequent star formation, which is believed to have been continuous throughout the lifetime of the Galaxy. Star formation history in this area is thus important in determining the secular evolution of the GC. We present 3-D high-resolution hydrodynamic simulations of the CMZ that consider self-gravity, radiative cooling, and supernova feedback, and discuss the efficiency and role of the star formation in that region.
Copyright: Sungsoo Kim
 
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