TY - JOUR
T1 - Star cluster formation in a turbulent molecular cloud self-regulated by photoionization feedback
AU - Gavagnin, Elena
AU - Bleuler, Andreas
AU - Rosdahl, Joakim
AU - Teyssier, Romain
N1 - Funding Information:
We thank the anonymous referee for their thoughtful comments and helpful suggestions. This work is supported by the STARFORM Sinergia Project funded by the Swiss National Science Foundation. We would like to thank Sam Geen, Patrick Hennebelle andMichela Mapelli for useful discussions.
Publisher Copyright:
© 2017 The Authors.
PY - 2017
Y1 - 2017
N2 - Most stars in the Galaxy are believed to be formed within star clusters from collapsing molecular clouds. However, the complete process of star formation, from the parent cloud to a gas-free star cluster, is still poorly understood. We perform radiation-hydrodynamical simulations of the collapse of a turbulent molecular cloud using the RAMSES-RT code. Stars are modelled using sink particles, from which we self-consistently follow the propagation of the ionizing radiation. We study how different feedback models affect the gas expulsion from the cloud and how they shape the final properties of the emerging star cluster.We find that the star formation efficiency is lower for stronger feedback models. Feedback also changes the high-mass end of the stellar mass function. Stronger feedback also allows the establishment of a lower density star cluster, which can maintain a virial or sub-virial state. In the absence of feedback, the star formation efficiency is very high, as well as the final stellar density. As a result, high-energy close encounters make the cluster evaporate quickly. Other indicators, such as mass segregation, statistics of multiple systems and escaping stars confirm this picture. Observations of young star clusters are in best agreement with our strong feedback simulation.
AB - Most stars in the Galaxy are believed to be formed within star clusters from collapsing molecular clouds. However, the complete process of star formation, from the parent cloud to a gas-free star cluster, is still poorly understood. We perform radiation-hydrodynamical simulations of the collapse of a turbulent molecular cloud using the RAMSES-RT code. Stars are modelled using sink particles, from which we self-consistently follow the propagation of the ionizing radiation. We study how different feedback models affect the gas expulsion from the cloud and how they shape the final properties of the emerging star cluster.We find that the star formation efficiency is lower for stronger feedback models. Feedback also changes the high-mass end of the stellar mass function. Stronger feedback also allows the establishment of a lower density star cluster, which can maintain a virial or sub-virial state. In the absence of feedback, the star formation efficiency is very high, as well as the final stellar density. As a result, high-energy close encounters make the cluster evaporate quickly. Other indicators, such as mass segregation, statistics of multiple systems and escaping stars confirm this picture. Observations of young star clusters are in best agreement with our strong feedback simulation.
KW - Galaxies: star clusters: general
KW - Galaxies: star clusters: individual: (NGC 3603 YC, Arches)
KW - Stars: formation
KW - Stars: kinematics and dynamics -HII regions
KW - Ultraviolet: stars
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U2 - 10.1093/MNRAS/STX2222
DO - 10.1093/MNRAS/STX2222
M3 - Article
AN - SCOPUS:85038884290
SN - 0035-8711
VL - 472
SP - 4155
EP - 4172
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -