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Numerical modeling of multiphase, turbulent galactic disks with star formation feedback

Published online by Cambridge University Press:  05 March 2015

Chang-Goo Kim ,
Eve C. Ostriker  and
Woong-Tae Kim
Chang-Goo Kim
Affiliation:
Department of Physics & Astronomy, Western University, Canada email: ckim256@uwo.ca
Eve C. Ostriker
Affiliation:
Department of Astronomy, University of Maryland, USA Astrophysical Sciences, Princeton University, USA
Woong-Tae Kim
Affiliation:
Department of Physics & Astronomy, Seoul National University, Republic of Korea
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Abstract

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Star formation is self-regulated by its feedback that drives turbulence and heats the gas. In equilibrium, the star formation rate (SFR) should be directly related to the total (thermal plus turbulent) midplane pressure and hence the total weight of the diffuse gas if energy balance and vertical dynamical equilibrium hold simultaneously. To investigate this quantitatively, we utilize numerical hydrodynamic simulations focused on outer-disk regions where diffuse atomic gas dominates. By analyzing gas properties at saturation, we obtain relationships between the turbulence driving and dissipation rates, heating and cooling rates, the total midplane pressure and the total weight of gas, and the SFR and the total midplane pressure. We find a nearly linear relationship between the SFR and the midplane pressure consistent with the theoretical prediction.

Keywords

stars: formationISM: kinematics and dynamicsmethods: numericalturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Highlights H16: Highlights of Astronomy , August 2012 , pp. 609 - 610
Copyright
Copyright © International Astronomical Union 2015 

References

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