Structure of molecular clouds. V - Detailed models and observational characteristics

Details Structure of molecular clouds. V - Detailed models and observational characteristics Structure of molecular clouds. V - Detailed models and observational characteristics

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...249..152s&link_type=abstract

Astrophysical Journal, Part 1, vol. 249, Oct. 1, 1981, p. 152-160. Deutsche Forschungsgemeinschaft

Astronomy and Astrophysics

Astrophysics

14

Astronomical Models, Interstellar Gas, Molecular Clouds, Stellar Evolution, Carbon Monoxide, Gravitational Collapse, Isotope Effect, Magnetohydrodynamic Waves, Plasma Chemistry, Propagation Velocity, Stellar Magnetic Fields, Turbulence Effects, Vapor Phases

Scientific paper

A detailed model of centrally condensed clouds containing regions of active star formation is derived from observations. The model has nearly equal turbulent and systematic collapse velocities and indicates that such clouds are not clumpy. Alfvenic waves can explain the turbulent velocities if the magnetic field varies as nH/2 to the 1/2 power. The model indicates the importance of chemical isotopic fractionation in CO, and suggests that metals play an important role in the ionization balance.

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