Collisional mergers and fragmentation of interstellar clouds

Astronomy and Astrophysics – Astrophysics

Scientific paper

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Hydrodynamic Equations, Hydrogen Clouds, Interstellar Matter, Molecular Collisions, Stellar Motions, Computer Programs, Gas Pressure, Gravitational Collapse, Hydrogen Atoms, Mass Ratios, Radiative Transfer, Spatial Resolution

Scientific paper

Collisions of interstellar H I clouds were simulated in three dimensions using a finite-particle hydrodynamics code. Interstellar clouds are not typically in detailed pressure balance with the intercloud medium, although their time-averaged pressure may be similar to the external value. Reasonable variations in radiative heating and cooling rates can alter the early stages of a high-speed collision but have rather minor effect on the end result. Collisions at the speeds characterized by a cloud velocity dispersion of 10 km/s are usually disruptive, often resulting in expanding systems which resemble observed filamentary clouds. A pair of colliding clouds is more likely to merge into one if the collision is at low relative velocity or the clouds are of greatly unequal mass.

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