Chemical equilibrium from diffuse to dense interstellar clouds. III - The model of the diffuse cloud Zeta Ophiuchi revisited

Details Chemical equilibrium from diffuse to dense interstellar clouds. III - The model of the diffuse cloud Zeta Ophiuchi revisited Chemical equilibrium from diffuse to dense interstellar clouds. III - The model of the diffuse cloud Zeta Ophiuchi revisited

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...190..215v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 190, no. 1-2, Jan. 1988, p. 215-236.

Astronomy and Astrophysics

Astrophysics

49

Astronomical Models, Chemical Equilibrium, Interstellar Chemistry, Molecular Clouds, Ophiuchi Clouds, Carbon Compounds, Hydroxyl Radicals, Molecular Excitation, Oscillator Strengths, Ultraviolet Radiation

Scientific paper

A steady state model of the chemical composition of interstellar clouds is used to ascertain the physical conditions prevailing in the diffuse cloud in front of the star Zeta Ophiuchii and in its environment. The chemical reaction scheme involves 1092 reactions among 85 chemical species; the chemistry of the deuterated species D, D(+), HD, HD(+), and H2D(+) is added to the chemical network. Photoabsorption and photodissociation rates for each individual line of the Lyman and Werner band of H2 and HD are computed as a function of depth in the cloud by solving a transfer equation for each line which takes all possible absorbers into account. This results in very efficient UV radiation shielding and leads to a transition from H to H2 which is more rapid than in previous models.

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