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What Species Remain to be Seen?

Published online by Cambridge University Press:  07 August 2017

B. E. Turner*
Affiliation:
National Radio Astronomy Observatory Charlottesville, Virginia, U.S.A.

Abstract

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We review what species remain to be seen for several types of astrochemistry: Thermochemical Equilibrium (TE) in circumstellar envelopes (CSEs); photo- and ion-molecule chemistry in CSEs; ion-molecule chemistry in cold interstellar clouds; grain chemistry (passive, catalytic, disruptive); and shock chemistry. In CSEs, a rich Si gas-phase chemistry is now recognized, and two predicted species (SiN, SiH2) have been seen. Others are predicted. In the ISM, a global picture of refractory-element chemistry predicts that compounds of Mg, Na, Fe, and possibly Al occur with detectable gas-phase abundance. Predicted species require laboratory synthesis and spectroscopy. Reactions of hydrocarbon ions with neutral species dominate the formation of the families CnH, HCnN, H2Cn, and CnO in both interstellar (TMC-1) and circumstellar (IRC10216) cases, and readily explain the favored values of n in each case as well as predicting which higher-n species remain to be seen. Confirmation of H3O+ (interstellar) is discussed.

Type
Quiescent Clouds and Regions of Star Formation
Copyright
Copyright © Kluwer 1992 

References

REFERENCES

Adams, N.G., Smith, D., Giles, D., and Herbst, E. 1989, A.&A. 220, 269 Google Scholar
Burton, M.G., Hollenbach, D., Haas, M., and Erickson, E. 1990, ApJ. 355, 197 CrossRefGoogle Scholar
Federman, S.R., and Allen, M. 1991, ApJ. 375, 157 CrossRefGoogle Scholar
Glassgold, A.E., Lucas, R., and Omont, A. 1986, A.&A. 157, 35 Google Scholar
Herbst, E., and Leung, C.M. 1989, ApJS 69, 271 Google Scholar
Herbst, E., Millar, T.J., Wlodek, S., and Bohme, D.K. 1989, A.&A. 222, 205 Google Scholar
Iguchi, T. 1975, Publ. Astron. Soc. Jpn. 27, 515 Google Scholar
Leger, A., Jura, M., and Omont, A. 1985, A.&A. 144, 147 Google Scholar
Meyers, D.M., and Roth, K.C. 1991, ApJL. (August 1) Google Scholar
Millar, T.J., Olofsson, H., Hjalmarson, A., and Brown, P. 1988, A.&A. 205, L5 Google Scholar
Millar, T.J. 1990, in From Ground-Based to Space-Borne Sub-mm Astronomy , Ed. Kaldeich, B. (Nordwijk: ESTEC), p. 233 Google Scholar
Neufeld, D.A., and Dalgarno, A. 1989, ApJ. 340, 689 Google Scholar
Seab, G.C. 1987, in Interstellar Processes , Eds. Hollenbach, D.J. and Thronson, H.A. (Dordrecht: Reidel), p.491 Google Scholar
Tarafdar, S.P. 1987, in Astrochemistry , Eds. Vardya, M.S. and Tarafdar, S.P., D. Reidel Google Scholar
Tielens, A.G.G.M. 1983, A.&A. 119, 137 Google Scholar
Tielens, A.G.G.M. 1990, in Chemistry and Spectroscopy of Interstellar Molecules , Ed. Kaifu, N., Univ. of Tokyo Press Google Scholar
Tsuji, T. 1973, A.&A. 23, 411 Google Scholar
Tsuji, T. 1987, in Astrochemistry , Eds. Vardya, M.S. and Tarafdar, S.P., D. Reidel Google Scholar
Tsuji, T. 1991, private communication Google Scholar
Turner, B.E. 1989, Space Sci. Reviews 51, 235 Google Scholar
Turner, B.E. 1990a, in Chemistry and Spectroscopy of Interstellar Molecules , Ed. Kaifu, N., Univ. of Tokyo Press Google Scholar
Turner, B.E. 1990b, ApJL 362, L29 Google Scholar
Turner, B.E. 1991a, ApJS 76, 617 Google Scholar
Turner, B.E. 1991b, ApJL submitted Google Scholar
Turner, B.E., Tsuji, T., Bally, J., Guelin, M., and Cernicharo, J. 1990, ApJ. 365, 569 Google Scholar
Turner, B.E., and Lubowich, D.A. 1991, ApJ. (Oct. 20) Google Scholar
Turner, B.E., and Steimle, T.C. 1991, in preparation Google Scholar
van Dishoeck, E., and Phillip, T.C. 1991, this symposium Google Scholar
Viala, Y.P. 1986, A.&A. Suppl. 64, 391 Google Scholar
Wootten, H.A., Mangum, J.G., Turner, B.E., Bogey, M., Boulanger, F., Combes, F., Encrenaz, P.J., and Gerin, M. 1991, ApJL in press Google Scholar