Volume 374, Number 3, August II 2001
|Page(s)||839 - 860|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 August 2001|
Numerical simulation of the formation of a spiral galaxy
Department of Physics and Astronomy, Cardiff University, PO Box 913, Cardiff, CF2 3YB, UK
2 Astronomical Institute, Tohoku University, Aoba, Sendai, 980-8578, Japan
3 Department of Physics and Astronomy, Cardiff University, PO Box 913, Cardiff, CF2 3YB, UK e-mail: firstname.lastname@example.org
Corresponding author: P. R. Williams, email@example.com
Accepted: 2 May 2001
A simulation is described in which the numerical galaxy formed compares favourably in every measurable respect with contemporary bright spiral galaxies, including the formation of a distinct stellar bulge and large scale spiral arm shocks in the gas component. This is achieved in spite of the fact that only idealized proto-galactic initial conditions were used, and only simple phenomenological prescriptions for the physics of the interstellar medium (ISM) and star formation were implemented. In light of the emphasis in recent literature on the importance of the link between galaxy formation and models of the universe on cosmological scales, on the details of the physics of the ISM and star formation, and on apparent problems therein, the implications of this result are discussed.
Key words: galaxies: spiral, formation, evolution, kinematics and dynamics, fundamental parameters / methods: N / body simulations
© ESO, 2001
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