Abstract
Work on three problems concerning the chemistry and dynamics of star forming fregions is addressed. Most of the work was done in collaboration with David A. Williams. A chemical model of core D ofTMC-1 is described; it is consistent with that dense core having evolved to its present physical state in the last 105years. Slow-mode wave excitation by the nonlinear evolution of fast-mode waves is examined as a possible mechanism for the production of structures, including densecores, in molecular sources. Sufficient atomic hydrogen may be present at the births of some dense cores that the radiative association of O with H is important in the initiation of the gas phase chemistry.
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Hartquist, T. Dynamical Molecular Regions in Interstellar Clouds. Astrophysics and Space Science 285, 717–724 (2003). https://doi.org/10.1023/A:1026121629121
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DOI: https://doi.org/10.1023/A:1026121629121