Chemodynamical Modelling of Galaxy Formation and Evolution |
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Authors: | Peter Berczik Gerhard Hensler Christian Theis Rainer Spurzem |
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Institution: | (1) Main Astronomical Observatory of Ukrainian National Academy of Sciences, Zabolotnoho Str. 27, 03680 Kiev, Ukraine;(2) Astronomisches Rechen-Institut, Heidelberg, Germany;(3) Institut für Theoretische Physik und Astrophysik, University of Kiel, Germany |
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Abstract: | We present our recently developed 3-dimensional chemodynamical code for galaxy evolution. This code follows the evolution
of different galactic components like stars, dark matter and different components of the interstellar medium (ISM), i.e. a
diffuse gaseous phase and the molecular clouds. Stars and dark matter are treated as collisionless N-body systems. The ISM
is numerically described by a smoothed particle hydrodynamics (SPH) approach for the diffuse gas and a sticky particle scheme
for the molecular clouds. Additionally, the galactic components are coupled by several phase transitions like star formation,
stellar death or condensation and evaporation processes within the ISM. As an example we show the dynamical and chemical evolution
of a star forming dwarf galaxy with a total baryonic mass of 2 ċ 109 M⊙. After a moderate collapse phase the stars and the molecular clouds follow an exponential radial distribution, whereas the
diffuse gas shows a central depression as a result of stellar feedback. The metallicities of the galactic components behave
quite differently with respect to their temporal evolution as well as their radial distribution. Especially, the ISM is at
no stage well mixed.
This revised version was published online in September 2006 with corrections to the Cover Date. |
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Keywords: | SPH chemodynamics dwarf galaxy evolution |
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