SFTISM
Star Formation in the Turbulent Interstellar Medium
| Coordinatore | UNIVERSITAT DE BARCELONA
Organization address
address: GRAN VIA DE LES CORTS CATALANES 585 contact info |
| Nazionalità Coordinatore | Spain [ES] |
| Totale costo | 100˙000 € |
| EC contributo | 100˙000 € |
| Programma | FP7-PEOPLE
Specific programme "People" implementing the Seventh Framework Programme of the European Community for research, technological development and demonstration activities (2007 to 2013) |
| Code Call | FP7-PEOPLE-2010-RG |
| Funding Scheme | MC-IRG |
| Anno di inizio | 2011 |
| Periodo (anno-mese-giorno) | 2011-01-01 - 2014-12-31 |
Partecipanti
| # | ||||
|---|---|---|---|---|
| 1 |
UNIVERSITAT DE BARCELONA
Organization address
address: GRAN VIA DE LES CORTS CATALANES 585 contact info |
ES (BARCELONA) | coordinator | 100˙000.00 |
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Obiettivo del progetto (Objective)
'The objective of this research project is to constrain star formation models with high dynamic range simulations. Current star formation simulations are based on unphysical initial conditions or artificial driving forces that mimic the energy injection from a large-scale turbulent cascade. This project proposes to overcome this limitation by developing star formation simulations that resolve the collapse of individual protostellar cores, while including the large scale-physical processes that drive the turbulence and control the life cycle of star-forming clouds. The project will include the large-scale physics by embedding the star-formation simulations, reaching a resolution of 200AU in collapsing cores, in a 1x1x20 Kpc region perpendicular to the Galactic disk. The ISM in this region will be modeled using three-dimensional, compressible, ideal MHD simulations (using adaptive mesh refinement methods), including density stratification in the Galactic gravitational field, gas self-gravity, radiative cooling, photoelectric and cosmic-ray heating, large-scale Galactic shear, star formation, and thermal and mechanical feedback from Type Ia, Ibc, and Type II SN explosions. Besides the derivation of the star formation rate and the stellar mass function, our simulations will provide large samples of star-forming clouds. We will analyze the physical properties of these clouds and will generate simulated observations through radiative transfer calculations of the cloud line and dust continuum emission. Results from this project will be relevant to studies of the formation and evolution of galaxies and to the star formation history of the universe. They will be used to formulate sub-grid models for cosmological simulations of galaxy formation, where stellar feedbacks are important. Our simulated observations of star-forming clouds will be valuable for the interpretation of real observations.'