Abstract
To understand the impact of radiation feedback during the formation of a globular cluster (GC), we simulate a head-on collision of two turbulent giant molecular clouds (GMCs). A series of idealized radiation-hydrodynamic simulations is performed, with and without stellar radiation or Type II supernovae. We find that a gravitationally bound, compact star cluster of mass M GC ∼ 105 M ⊙ forms within ≈3 Myr when two GMCs with mass M GMC = 3.6 × 105 M ⊙ collide. The GC candidate does not form during a single collapsing event but emerges due to the mergers of local dense gas clumps and gas accretion. The momentum transfer due to the absorption of the ionizing radiation is the dominant feedback process that suppresses the gas collapse, and photoionization becomes efficient once a sufficient number of stars form. The cluster mass is larger by a factor of ∼2 when the radiation feedback is neglected, and the difference is slightly more pronounced (16%) when extreme Lyα feedback is considered in the fiducial run. In the simulations with radiation feedback, supernovae explode after the star-forming clouds are dispersed, and their metal ejecta are not instantaneously recycled to form stars.
| Original language | English |
|---|---|
| Article number | 53 |
| Journal | Astrophysical Journal |
| Volume | 935 |
| Issue number | 1 |
| DOIs | |
| Publication status | Published - 2022 Aug 1 |
Bibliographical note
Funding Information:T.K. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (Nos. 2020R1C1C1007079 and 2022R1A6A1A03053472), and acted as the corresponding author. The supercomputing time for numerical simulations was kindly provided by KISTI (KSC-2019-CRE-0196), and large data transfer was supported by KREONET, which is managed and operated by KISTI. This work was also performed using the DiRAC Data Intensive service at Leicester, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). The equipment was funded by BEIS capital funding via STFC capital grants ST/K000373/1 and ST/R002363/1 and STFC DiRAC Operations grant ST/R001014/1. DiRAC is part of the National e-Infrastructure.
Funding Information:
T.K. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (Nos. 2020R1C1C1007079 and 2022R1A6A1A03053472), and acted as the corresponding author. The supercomputing time for numerical simulations was kindly provided by KISTI (KSC-2019-CRE-0196), and large data transfer was supported by KREONET, which is managed and operated by KISTI. This work was also performed using the DiRAC Data Intensive service at Leicester, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility ( www.dirac.ac.uk ). The equipment was funded by BEIS capital funding via STFC capital grants ST/K000373/1 and ST/R002363/1 and STFC DiRAC Operations grant ST/R001014/1. DiRAC is part of the National e-Infrastructure.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science