High-mass star formation in the Large Magellanic Cloud triggered by colliding H I flows

The galactic tidal interaction is a possible mechanism to trigger active star formation in galaxies. Recent analyses using H I data in the Large Magellanic Cloud (LMC) proposed that the tidally driven H I 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, and the 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 pressure may be a key parameter in star formation.