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Modelling Galaxies with a 3D Multi-Phase ISM

Published online by Cambridge University Press:  05 March 2013

Stefan Harfst ,
Christian Theis  and
Gerhard Hensler
Stefan Harfst*
Affiliation:
University of Kiel, Institute of Theoretical Physics and Astrophysics, 24098 Kiel, Germany Centre for Astrophysics & Supercomputing, Swinburne University, VIC 3122, Australia
Christian Theis
Affiliation:
University of Kiel, Institute of Theoretical Physics and Astrophysics, 24098 Kiel, Germany University of Vienna, Institute of Astronomy, 1180 Vienna, Austria
Gerhard Hensler
Affiliation:
University of Kiel, Institute of Theoretical Physics and Astrophysics, 24098 Kiel, Germany University of Vienna, Institute of Astronomy, 1180 Vienna, Austria
*
4E-mail: harfst@astrophysik.uni-kiel.de
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Abstract

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We present a modified TREE-SPH code to model galaxies in three dimensions. The model includes a multi-phase description of the interstellar medium which combines two numerical techniques. A diffuse warm/hot gas phase is modelled by SPH, whereas a cloudy medium is represented by a sticky particle scheme. Interaction processes (such as star formation and feedback), cooling, and mixing by condensation and evaporation, are taken into account. Here we apply our model to the evolution of a Milky Way type galaxy. After an initial stage, a quasi-equilibrium state is reached. It is characterised by a star formation rate of ∼1 M⊙ yr–1. Condensation and evaporation rates are in balance at 0.1–1 M⊙ yr–1.

Keywords

galaxies: ISM, evolutionISM: evolution; kinematics and dynamicsmethods: N-body simulations
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 21 , Issue 2: The Fifth Workshop on Galactic Chemodynamics , 2004 , pp. 228 - 231
Copyright
Copyright © Astronomical Society of Australia 2004

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