Simulating star clusters across cosmic time: I. Initial mass function, star formation rates, and efficiencies
We present radiation-magneto-hydrodynamic simulations of star formation in self-gravitating, turbulent molecular clouds, modelling the formation of individual massive stars, including their UV radiation feedback.
Saved in:
| Main Authors: | , , |
|---|---|
| Format: | Article (Journal) |
| Language: | English |
| Published: |
2019 April 2
|
| In: |
Monthly notices of the Royal Astronomical Society
Year: 2019, Volume: 489, Issue: 2, Pages: 1880-1898 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stz2239 |
| Online Access: | Verlag, Volltext: https://doi.org/10.1093/mnras/stz2239 Verlag: https://academic.oup.com/mnras/article/489/2/1880/5548825 
|
| Author Notes: | Chong-Chong He, Massimo Ricotti and Sam Geen |
| Summary: | We present radiation-magneto-hydrodynamic simulations of star formation in self-gravitating, turbulent molecular clouds, modelling the formation of individual massive stars, including their UV radiation feedback. |
|---|---|
| Item Description: | Gesehen am 28.10.2019 |
| Physical Description: | Online Resource |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stz2239 |