FORMATION OF MASSIVE MOLECULAR CLOUD CORES BY CLOUD–CLOUD COLLISION

@article{Inoue2013FORMATIONOM,
  title={FORMATION OF MASSIVE MOLECULAR CLOUD CORES BY CLOUD–CLOUD COLLISION},
  author={Tsuyoshi Inoue and Yasuo Fukui},
  journal={The Astrophysical Journal Letters},
  year={2013},
  volume={774}
}
Recent observations of molecular clouds around rich massive star clusters including NGC 3603, Westerlund 2, and M20 revealed that the formation of massive stars could be triggered by a cloud–cloud collision. By using three-dimensional, isothermal, magnetohydrodynamics simulations with the effect of self-gravity, we demonstrate that massive, gravitationally unstable, molecular cloud cores are formed behind the strong shock waves induced by cloud–cloud collision. We find that the massive… 

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References

SHOWING 1-10 OF 47 REFERENCES

FORMATION OF TURBULENT AND MAGNETIZED MOLECULAR CLOUDS VIA ACCRETION FLOWS OF H i CLOUDS

Using three-dimensional magnetohydrodynamic simulations, including the effects of radiative cooling/heating, chemical reactions, and thermal conduction, we investigate the formation of molecular

Molecular Cloud Evolution

I describe the scenario of molecular cloud (MC) evolution that has emerged over the past decade or so. MCs can start out as cold atomic clouds formed by compressive motions in the warm neutral medium

Was a cloud-cloud collision the trigger of the recent star formation in Serpens?

Context. The complexity of the interstellar medium (ISM) is such that it is unlikely that star formation is initiated in the same way in all molecular clouds. While some clouds seem to collapse on

THE FRAGMENTATION OF MAGNETIZED, MASSIVE STAR-FORMING CORES WITH RADIATIVE FEEDBACK

We present a set of three-dimensional, radiation-magnetohydrodynamic calculations of the gravitational collapse of massive (300 M☉), star-forming molecular cloud cores. We show that the combined

Collapse, outflows and fragmentation of massive, turbulent and magnetized prestellar barotropic cores

Context. Stars, and more particularly massive stars, have a drastic impact on galaxy evolution. Yet the conditions in which they form and collapse are still not fully understood. Aims: In

The Formation of Massive Star Systems by Accretion

Three-dimensional radiation-hydrodynamic simulations of the collapse of a massive prestellar core are presented and it is found that radiation pressure does not halt accretion, but the instabilities that allow accretion to continue lead to small multiple systems.

MOLECULAR CLOUDS TOWARD THE SUPER STAR CLUSTER NGC 3603; POSSIBLE EVIDENCE FOR A CLOUD–CLOUD COLLISION IN TRIGGERING THE CLUSTER FORMATION

We present new large field observations of molecular clouds with NANTEN2 toward the super star cluster NGC 3603 in the transitions 12CO(J = 2–1, J = 1–0) and 13CO(J = 2–1, J = 1–0). We suggest that

A minimum column density of 1 g cm-2 for massive star formation

It is shown that only clouds with column densities of at least 1 g cm-2 can avoid fragmentation and form massive stars, and the existence of a threshold implies that the initial mass function should show detectable variation with environment within the Galaxy.

On the Formation of Massive Stars

We calculate numerically the collapse of slowly rotating, nonmagnetic, massive molecular clumps of masses 30, 60, and 120 M☉, which conceivably could lead to the formation of massive stars. Because

TOWARD UNDERSTANDING THE COSMIC-RAY ACCELERATION AT YOUNG SUPERNOVA REMNANTS INTERACTING WITH INTERSTELLAR CLOUDS: POSSIBLE APPLICATIONS TO RX J1713.7−3946

Using three-dimensional magnetohydrodynamic simulations, we investigate general properties of a blast wave shock interacting with interstellar clouds. The pre-shock cloudy medium is generated as a