Copernicus observations of C I and CO in diffuse interstellar clouds

Details Copernicus observations of C I and CO in diffuse interstellar clouds Copernicus observations of C I and CO in diffuse interstellar clouds

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980usc..rept.....j&link_type=abstract

Final Technical Report, 14 Mar. 1977 - 13 Nov. 1980 University of Southern California, Los Angeles. Dept. of Astronomy.

Astronomy and Astrophysics

Astronomy

Astronomical Observatories, Carbon Isotopes, Carbon Monoxide, Clouds, Line Spectra, Oao 3, Absorption Spectra, Astronomy, Interstellar Gas, Thermal Radiation

Scientific paper

Copernicus was used to observe absorption lines of C I in its ground state and excited fine structure levels and CO toward 29 stars. We use the C I data to infer densities and pressures within the observed clouds, and because our results are of higher precision than previous work, much more precise estimates of the physical conditions in clouds are obtained. In agreement with previous work, the interstellar thermal pressure appears to be variable, with most clouds having values of p/k between 1000/cu cm K and 10,000/cu cm K, but there are some clouds with p/k as high as 100,000/cu cm K. Our results are consistent with the view that the interstellar thermal pressure is so variable that the gas undergoes continuous dynamic evolution. Our observations provide useful constraints on the physical processes on the surfaces of grains. In particular, we find that grains are efficient catalysts of interstellar H2 in the sense that at least half of the hydrogen atoms that strike grains come off as part of H2. Results place strong constraints on models for the formation and destruction of interstellar CO. In many clouds, an order of magnitude less CO than predicted in some models was found.

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