# Formation of the Young Massive Cluster R136 triggered by Tidally-driven Colliding HI Flows

## TL;DR

This paper proposes that the formation of the young massive cluster R136 was triggered by a collision between two HI gas components in the LMC, driven by tidal interactions with the SMC, supported by observational and simulation data.

## Contribution

It introduces a new hypothesis linking tidal-driven colliding HI flows to the formation of R136 and surrounding high-mass stars in the LMC.

## Key findings

- Identification of colliding HI components near R136
- Evidence of bridge features and complementary distributions
- A proposed formation mechanism involving shock compression

## Abstract

Understanding of massive cluster formation is one of the important issues of astronomy. By analyzing the HI data, we have identified that the two HI velocity components (L- and D-components) are colliding toward the HI Ridge, in the southeastern end of the LMC, which hosts the young massive cluster R136 and $\sim$400 O/WR stars (Doran et al. 2013) including the progenitor of SN1987A. The collision is possibly evidenced by bridge features connecting the two HI components and complementary distributions between them. We frame a hypothesis that the collision triggered the formation of R136 and the surrounding high-mass stars as well as the HI & Molecular Ridge. Fujimoto & Noguchi (1990) advocated that the last tidal interaction between the LMC and the SMC about 0.2 Gyr ago induced collision of the L- and D-components. This model is consistent with numerical simulations (Bekki & Chiba 2007b). We suggest that a dense HI partly CO cloud of 10$^{6}$ $M_{\odot}$, a precursor of R136, was formed at the shock-compressed interface between the colliding L- and D-components. We suggest that part of the low-metalicity gas from the SMC was mixed in the tidal interaction based on the $Planck/IRAS$ data of dust optical depth (Planck Collaboration et al. 2014).

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Source: https://tomesphere.com/paper/1703.01075