Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....65..435c&link_type=abstract
Astronomy and Astrophysics, vol. 65, no. 3, May 1978, p. 435-448.
Astronomy and Astrophysics
Astrophysics
48
Chemical Equilibrium, Cosmic Gases, Interstellar Chemistry, Interstellar Matter, Stellar Evolution, Thermodynamic Equilibrium, Abundance, Angular Velocity, Carbon Monoxide, Chemical Composition, Hydrogen Clouds, Magnetic Flux, Photoionization, Radiant Cooling, Radiative Heat Transfer, Steady State, Ultraviolet Radiation
Scientific paper
The theory of gravitational contraction of interstellar matter is used as the basis for a steady-state model of chemical and thermal equilibrium in dense dark clouds. Attention is given to the evolutionary path of the clouds, in which pressure gradients and electron density are the most important parameters. Interstellar abundances are considered, e.g., C, C/+/, CO, CH, OH, H2O, O2, together with formation on grains in gas phase reactions. It is noted that gas-grain collisions are relatively unimportant as a heating mechanism; heating being effected chiefly through cosmic ray ionization of H2 and the H2 formation of grains. A gas temperature of 10 K is assumed for the inner parts of the cloud, and the transfer equation of UV radiation is solved in a manner consistent with the chemical and thermal balance equations.
Bel N.
Clavel Jean
Viala Y. P.
No associations
LandOfFree
Chemical and thermal equilibrium in dark clouds does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Chemical and thermal equilibrium in dark clouds, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Chemical and thermal equilibrium in dark clouds will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1295307