Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...245...72h&link_type=abstract
Astrophysical Journal, Part 1, vol. 245, Apr. 1, 1981, p. 72-91.
Astronomy and Astrophysics
Astrophysics
75
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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