Skip to main content

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

Author(s): Kim, CG; Ostriker, Eve C; Kim, WT

To refer to this page use:
Full metadata record
DC FieldValueLanguage
dc.contributor.authorKim, CG-
dc.contributor.authorOstriker, Eve C-
dc.contributor.authorKim, WT-
dc.identifier.citationKim, CG, Ostriker, EC, Kim, WT. (2012). Numerical modeling of multiphase, turbulent galactic disks with star formation feedback. Proceedings of the International Astronomical Union, 10 (H16), 609 - 610. doi:10.1017/S174392131401240Xen_US
dc.description.abstractStar 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.en_US
dc.format.extent609 - 610en_US
dc.relation.ispartofProceedings of the International Astronomical Unionen_US
dc.rightsAuthor's manuscripten_US
dc.subjectstars: formation, ISM: kinematics and dynamics, methods: numerical, turbulenceen_US
dc.titleNumerical modeling of multiphase, turbulent galactic disks with star formation feedbacken_US
dc.typeJournal Articleen_US

Files in This Item:
File Description SizeFormat 
1211.5161v1.pdf374.76 kBAdobe PDFView/Download

Items in OAR@Princeton are protected by copyright, with all rights reserved, unless otherwise indicated.