High-mass star formation in the Large Magellanic Cloud triggered by colliding HI flows
Abstract
The galactic tidal interaction is a possible mechanism to trigger the active star formation in galaxies. The recent analyses using the HI data in the Large Magellanic Cloud (LMC) proposed that the tidally driven HI flow, the L-component, is colliding with the LMC disk, the D-component, and is triggering high-mass star formation toward the active star-forming regions R136 and N44. In order to explore the role of the collision over the entire LMC disk, we investigated the I-component, the collision-compressed gas between the L- and D-components, over the LMC disk, and found that 74% of the O/WR stars are located toward the I-component, suggesting their formation in the colliding gas. We compared four star-forming regions (R136, N44, N11, N77-N79-N83 complex). We found a positive correlation between the number of high-mass stars and the compressed gas pressure generated by collisions, suggesting that the pressure may be a key parameter in star formation.
Keywords
Cite
@article{arxiv.2405.05046,
title = {High-mass star formation in the Large Magellanic Cloud triggered by colliding HI flows},
author = {K. Tsuge and H. Sano and K. Tachihara and K. Bekki and K. Tokuda and T. Inoue and N. Mizuno and A. Kawamura and T. Onishi and Y. Fukui},
journal= {arXiv preprint arXiv:2405.05046},
year = {2024}
}
Comments
33 pages, 18 figures, 3 Tables, accepted for publication in PASJ. arXiv admin note: text overlap with arXiv:2010.08816