By Alexander J. W.

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Astrophys. Suppl. 119:111–114. , and Le Bourlot, J. 1996b. , Pineau des Forets, Photodissociation of H2 and CO and time dependent chemistry in inhomogeneous interstellar clouds. Astron. Astrophys. 311:690–707. , Walmsley, C. , Wilson, T. , and Muders, D. 1995. A detailed study of an extremely quiescent core: L 1498. Astron. Astrophys. 302:509– 520. Lepp, S.. 1992. The cosmic-ray ionization rate. In Astrochemistry of Cosmic Phenomena, ed. P. D. Singh (Dordrecht: Kluwer), pp. 471–475. McCall, B. , Geballe, T.

Abundances at earlier times compared to steady state, whereas SO has large concentrations in equilibrium. The reaction of SO with OH is expected to produce SO2 . However, the observed SO2 abundance is generally low in dark clouds, indicating an incomplete understanding of the sulfur chemistry and the depletion of sulfur (Palumbo et al. 1997). The above scenario leads to a dichotomy in the chemistry: 1. Species linked to the carbon chemistry, such as CS, CN, HCN, complex carbon chains, and organics, have larger abundances at earlier evolutionary stages.

Astrophys. J. 454:327– 344. Blake, G. , Sutton, E. , Masson, C. , and Phillips, T. G. 1987. Molecular abundances in OMC-1. The chemical composition of interstellar molecular clouds and the influence of massive star formation. Astrophys. J. 315:621– 645. Blake, G. , van Dishoeck, E. , and Sargent, A. 1992. Chemistry in circumstellar disks—CS toward HL Tauri. Astrophys. J. 391:L99–L103. Blake, G. , van Dishoeck, E. , Jansen, D. , and Mundy, L. G. 1994. Molecular abundances and low-mass star formation.

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A Matrix Knot Invariant by Alexander J. W.

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