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What Species Remain to be Seen?

Published online by Cambridge University Press:  07 August 2017

B. E. Turner
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 Cn H, HCn N, H2Cn , and Cn O 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.

Information

Type
Quiescent Clouds and Regions of Star Formation
Information
Symposium - International Astronomical Union , Volume 150: Astrochemistry of Cosmic Phenomena , 1992 , pp. 181 - 186
Copyright
Copyright © Kluwer 1992 

References

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