Astronomy & Astrophysics

Issue		A&A Volume 449, Number 2, April II 2006
Page(s)		509 - 518
Section		Extragalactic astronomy
DOI		10.1051/0004-6361:20042190

A&A 449, 509-518 (2006)
DOI: 10.1051/0004-6361:20042190

Modelling galaxies with a 3d multi-phase ISM

S. Harfst^{1, 2}, Ch. Theis^{1, 3} and G. Hensler³

¹ Institut für Theoretische Physik und Astrophysik, Universität Kiel, 24098 Kiel, Germany
e-mail: harfst@astrophysik.uni-kiel.de
² Centre for Astrophysics and Supercomputing, Swinburne University, Hawthorn, Victoria 3122, Australia
³ Institut für Astronomie, Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria

(Received 15 October 2004 / Accepted 11 November 2005 )

Abstract
We present a new particle code for modelling the evolution of galaxies. The code is based on a multi-phase description for the interstellar medium (ISM). We include star formation (SF), stellar feedback by massive stars and planetary nebulae, phase transitions, and interactions between gas clouds and ambient diffuse gas, namely condensation, evaporation, drag, and energy dissipation. The last is realised by radiative cooling and inelastic cloud-cloud collisions. We present new schemes for SF and stellar feedback that include a consistent calculation of the star-formation efficiency (SFE) based on ISM properties, as well as a detailed redistribution of the feedback energy into the different ISM phases.

As a first test we show a model of the evolution of a present day Milky-Way-type galaxy. Though the model exhibits a quasi-stationary behaviour in global properties like mass fractions or surface densities, the evolution of the ISM is strongly variable locally depending on the local SF and stellar feedback. We start only with two distinct phases, but a three-phase ISM is formed soon and consists of cold molecular clouds, a warm gas disk, and a hot gaseous halo. Hot gas is also found in bubbles in the disk accompanied by type II supernovae explosions. The volume-filling factor of the hot gas in the disk is ~ $35\%$ . The mass spectrum of the clouds follows a power-law with an index of $\alpha \approx -2$ . The star-formation rate (SFR) is ~ $1.6~\ensuremath_{\odot}} ~\ensuremath{\,{\rm yr}^}$ on average, decreasing slowly with time due to gas consumption. In order to maintain a constant SFR, gas replenishment, e.g. by infall, of the order $1~\ensuremath_{\odot}} ~\ensuremath{\,{\rm yr}^}$ is required. Our model is in fair agreement with Kennicutt's (1998, ApJ, 498, 541) SF law including the cut-off at ~ $10~\ensuremath_{\odot}} ~\ensuremath{{\rm pc}^}$ . Models with a constant SFE, i.e. no feedback on the SF, fail to reproduce Kennicutt's law.

We performed a parameter study varying the particle resolution, feedback energy, cloud radius, SF time scale, and metallicity. In most these cases the evolution of the model galaxy was not significantly different to our reference model. Increasing the feedback energy by a factor of 4-5 lowers the SF rate by ~ $0.5~\ensuremath_{\odot}} ~\ensuremath{\,{\rm yr}^}$ , while decreasing the metallicity by a factor of ~100 increases the mass fraction of the hot gas from about 10% to 30%.

Key words: methods: N-body simulations -- ISM: evolution -- Galaxy: evolution -- galaxies: ISM -- galaxies: kinematics and dynamics

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