Astronomy and Astrophysics – Astronomy
Scientific paper
May 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...444..708t&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 444, no. 2, p. 708-720
Astronomy and Astrophysics
Astronomy
18
Astronomical Models, Galactic Structure, Hydrostatics, Interstellar Matter, Molecular Clouds, Nitrogen Hydrides, Abundance, Galactic Structure, Line Spectra, Ultraviolet Astronomy, Vapor Phases
Scientific paper
We have made extensive observations of the (1, 1) and (2, 2) lines of NH3 in all 27 of the Clemens-Barvainis small molecular clouds for which several structural models including hydrostatic equilibrium polytropes were developed in an earlier paper based on CO-18 and (13)CO observations. As with the 11 cirrus cores earlier studied in CO-18, (13)CO, H2CO, and NH3, the NH3 lines in CB objects are well fitted by both polytropic models and ad hoc n is approximately 1/r models, using the external UV fields derived in the earlier papers. The reanalysis of the cirrus cores, which now includes the C-12/C-13 ratio as a variable, yields the same NH3 fractional abundances as the earlier analysis, and reaffirms a strong preference for centrally condensed abundance profiles. The same preference is found, but somewhat less decisively, for the CB objects. As before, the NH3 analyses give no clear preference for polytropic or 1/r structures. The large central NH3 abundances (0.4-3.2 x10-8 for cirrus cores; a factor 1.8 times smaller for CB objects) are much too large is these translucent objects to be explained by the standard gas-phase reaction N(+) + H2 approaches NH(+), but may be explained by the reaction N + H3(+) approaches NH2(+) provided it has no activation barrier. Various arguments are advanced against photcatalysis of NH3 on grains. By including consistently the effects of UV radiation fields and electron excitation, our models have now fitted accurately all four lines of CO-18 and (13)CO, three lines of H2CO, and two lines of NH3 so far observed. With the possible exception of the (average) NH3 abundances, the CB objects and cirrus cores are indistinguishable physically or chemically, and the properties we have found for them seem to represent the conditions in all small, low-mass moleculra clouds regardless of galactic latitude.
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