Formation and heating of molecular cloud cores.
Abstract
The origin of molecular cloud cores and their evolution into star-forming regions are discussed, reviewing the results of recent theoretical investigations. Numerical results are presented graphically, and it is argued that the existence and properties of self-gravitating clouds can be explained most easily by the action of magnetic fields. Supercritical and subcritical cloud regimes (where the cloud mass is greater or less, respectively, than the mass at which cloud self-gravity can overcome magnetic-field support) are defined and related to two types of star formation: (1) highly efficient star formation and (2) inefficient formation of low-mass stars. Mechanism (1) is shown to favor the formation of high-mass stars whenever significant core heating occurs (e.g., via ambipolar diffusion).
- Publication:
-
Physical Processes in Interstellar Clouds
- Pub Date:
- 1987
- DOI:
- 10.1007/978-94-009-3945-5_14
- Bibcode:
- 1987ASIC..210..173L
- Keywords:
-
- Astrophysics;
- Gas Heating;
- Molecular Clouds;
- Star Formation;
- Carbon Monoxide;
- Friction;
- Gravitational Collapse;
- Stellar Mass;
- Astrophysics;
- Magnetic Fields:Molecular Clouds;
- Molecular Clouds:Core Formation;
- Molecular Clouds:Heating;
- Molecular Clouds:Magnetic Fields;
- Molecular Clouds:Star Formation;
- Star Formation:Molecular Clouds