Collisional mergers and fragmentation of interstellar clouds
Abstract
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.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- April 1981
- DOI:
- 10.1086/158787
- Bibcode:
- 1981ApJ...245...72H
- Keywords:
-
- Hydrodynamic Equations;
- Hydrogen Clouds;
- Interstellar Matter;
- Molecular Collisions;
- Stellar Motions;
- Computer Programs;
- Gas Pressure;
- Gravitational Collapse;
- Hydrogen Atoms;
- Mass Ratios;
- Radiative Transfer;
- Spatial Resolution;
- Astrophysics