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Star formation and chemical evolution in smoothed particle hydrodynamics simulations: a statistical approach
Article first published online: 4 APR 2002
DOI: 10.1046/j.1365-8711.2002.05118.x
Issue
1365-2966/asset/cover.gif?v=1&s=2a3d0853ca0438b9cc112063a5fea6636d67d32e "Monthly Notices of the Royal Astronomical Society")
Monthly Notices of the Royal Astronomical Society
Volume 330, Issue 4, pages 821–836, March 2002
Additional Information
How to Cite
Lia, C., Portinari, L. and Carraro, G. (2002), Star formation and chemical evolution in smoothed particle hydrodynamics simulations: a statistical approach. Monthly Notices of the Royal Astronomical Society, 330: 821–836. doi: 10.1046/j.1365-8711.2002.05118.x
Publication History
- Issue published online: 4 APR 2002
- Article first published online: 4 APR 2002
- Accepted 2001 November 1. Received 2001 October 29; in original form 2001 March 8
- Abstract
- Article
- References
- Cited By
Keywords:
- hydrodynamics;
- methods: numerical;
- stars: formation;
- galaxies: evolution
In smoothed particle hydrodynamics (SPH) codes with a large number of particles, star formation as well as gas and metal restitution from dying stars can be treated statistically. This approach allows one to include detailed chemical evolution and gas re-ejection with minor computational effort. Here we report on a new statistical algorithm for star formation and chemical evolution, especially conceived for SPH simulations with large numbers of particles, and for parallel SPH codes.
For the sake of illustration, we also present two astrophysical simulations obtained with this algorithm, implemented into the Tree-SPH code by Lia & Carraro.
In the first simulation, we follow the formation of an individual disc-like galaxy, predict the final structure and metallicity evolution, and test resolution effects. In the second simulation we simulate the formation and evolution of a cluster of galaxies, to demonstrate the capabilities of the algorithm in investigating the chemo-dynamical evolution of galaxies and of the intergalactic medium in a cosmological context.