Three-Dimensional Numerical Simulation of Interstellar Cloud-Cloud Collisions and Triggered Star Formation. I ---Head-On Collisions---

Details Three-Dimensional Numerical Simulation of Interstellar Cloud-Cloud Collisions and Triggered Star Formation. I ---Head-On Collisions--- Three-Dimensional Numerical Simulation of Interstellar Cloud-Cloud Collisions and Triggered Star Formation. I ---Head-On Collisions---

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pthph..78.1250n&link_type=abstract

Progress of Theoretical Physics, Vol. 78, No. 6, pp. 1250-1272

Physics

22

Scientific paper

We simulate the head-on collisions between isothermal interstellar clouds by using a three-dimensional hydrodynamic code. The cloud-cloud collision is one of the important mechanisms which trigger star formation. We obtain a new dynamical criterion for the gravitational instability instead of the static criterion for the Bonnor-Ebert sphere. In the collision between identical clouds with relative velocity greater than the sound velocity, the chock compressed layer is formed and the central density increases by the square of the impact Mach number. As a result, the enhanced self-gravity induces the instability and the central part of the cloud begins to collapse even if the total mass is smaller than the Bonnor-Ebert critical mass M_{BE. The efficiency of this triggering mechanism, however, does not increase by far for the high Mach number collision because of the saturation of the gravity in disk geometry. In the head-on collision between hot clouds with small mass such as M < 0.4 M_{BE, they only merge and make a quadrupole oscillation around an equilibrium configuration.

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