Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.196...13i&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 196, July 1981, p. 13-22. Research supported by the Universidad de Los
Astronomy and Astrophysics
Astronomy
3
Fragmentation, Hydrogen, Interstellar Chemistry, Interstellar Matter, Protostars, Hydrogen Atoms
Scientific paper
The chemical equation for H2 formation (in nonequilibrium condition) and the energy equation were solved numerically like a two boundary value problem. The values of the chemical parameter x, the gas temperature p, and the mass density were obtained explicitly as functions of time and they were compared with the change in the mean density produced by the free-fall. The ability of H2 formation to act as a direct nonlinear amplifier of density inhomogeneities in prestellar clouds depends critically on the initial values of the number density of particles, the temperature, and the percentage of chemical heat input to the gas. In particular, if the remainder of the binding energy of H2 formation is radiated by the grains, H2 formation can induce fragmentation in a contracting cloud providing that the temperature is greater than 60 K and the q number density is greater then 100 per cu cm.
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