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The galactic tidal interaction is a possible mechanism to trigger the activestar formation in galaxies. Recent analyses using the Hi data in the LargeMagellanic Cloud (LMC) proposed that the tidally driven colliding HI flows,induced by the galactic interaction with the Small Magellanic Cloud (SMC),triggered high-mass star formation in the southeastern HI Ridge, including R136and $\sim$400 O/WR stars, and the galactic center region hosting the N44region. This study performed a comprehensive HI data analysis across the LMCand found that two Hi velocity components defined in the early studies (L- andD- components) are quasi-ubiquitous with signatures of interaction dynamicallytoward the other prominent HII regions, such as N11 and N79. We characterizethe intimidate velocity range (I-component) between the two components as thedecelerated gas by momentum conservation in the collisional interaction. Thespatial distributions of the I-component and those of the O/WR stars have goodagreements with each other whose fraction is more than $\sim$70% at a scale of$\sim$15 pc, which is significantly smaller than the typical GMC size. Based onthe results of our new simulations of the LMC-SMC interaction, we propose thatthe interaction about 0.2 Gyr ago induced efficient infall of gas from the SMCto the LMC and consequently ended up with recent formation of high-mass starsdue to collisions of HI gas in the LMC. The new numerical simulations of thegas dynamics successfully reproduce the current distribution of theL-component. This lends theoretical support for the present picture.

Active star formation across the whole Large Magellanic Cloud triggered by tidally-driven colliding HI flows