H2O and O2 have long been predicted to be major constituents of star-forming molecular gas. Line emission from these molecules are explored using the newest collisional excitation rate coefficients and the latest chemical and thermal profiles for shocks and photodissociation regions (PDRs) In the case of the PDRs, the parameters of FUV-illuminated gas in the molecular clouds, hydrogen density (n = 103-10 6H=cm3) and FUV flux intensity (g = 1 - 105 times the ambient interstellar field) are considered. In the case of shocks, shock velocities of 5 - 40 km/s and gas densities of 10 3-106.5H=cm3 are considered. The results are compared to existing intensity models of H2O and O2 in preparation for an analysis of future Herschel telescope observations. Line intensity results are consistent with similar models within an order of magnitude.
|Commitee:||Becker, Joseph F., Beyersdorf, Peter|
|School:||San Jose State University|
|School Location:||United States -- California|
|Source:||MAI 50/02M, Masters Abstracts International|
|Keywords:||Herschel, Oxygen, Photodissociation, Shocks, Spectra, Star-forming|
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