Laboratory Studies of Ion/Molecule Reactions of Fullerenes: Chemical Derivatization of Fullerenes within Dense Interstellar Clouds and Circumstellar Shells

2000 ◽  
Vol 540 (2) ◽  
pp. 869-885 ◽  
Author(s):  
Simon Petrie ◽  
Diethard K. Bohme

The rare stable isotopes of several elements (e.g. D, 13 C and 15 N) have been detected in several interstellar molecules, and their abundance relative to the more common isotope is often enhanced above that in the solar-terrestrial environment. Important questions to answer are to what extent the isotopic ratios in the molecules are representative of those in the cloud matter as a whole, and whether fractionation of the heavier isotope into the molecules via ion—molecule interactions is a significant process. A laboratory study of isotope exchange in ion-molecule reactions has therefore been carried out, the results of which indicate that fractionation of heavy isotopes can occur very efficiently at low temperatures. Consideration is given in this paper to reactions in which H-D, 12 C - 13 C, 14 N - 15 N and 16 O - 18 O exchange occurs, and it is shown how better estimates of the electron density and the temperature in interstellar clouds have been obtained from these laboratory data.


1980 ◽  
Vol 44 ◽  
pp. 481 ◽  
Author(s):  
W. T., Jr. Huntress ◽  
V. G. Anicich ◽  
M. J. McEwan ◽  
Z. Karpas

1980 ◽  
Vol 87 ◽  
pp. 311-315
Author(s):  
Nigel G. Adams ◽  
David Smith

From our laboratory data relating to several hundreds of ion-atom and ion-molecule reactions at thermal energies, we qualitatively describe probable chemical paths to the synthesis of amino-, cyano-and nitroso-compounds in interstellar clouds.


1980 ◽  
Vol 87 ◽  
pp. 299-303 ◽  
Author(s):  
M.J. Mcewan ◽  
V. G. Anicich ◽  
W.T. Huntress

Rate constants obtained by the ICR technique are reported for reaction (1), C2H2+ + HCN and reaction (2) HCN+ + C2H2 such that k1 = 3.6 × 10−10 and k2 = 6.9 × 10−10 cm3 molecule−1 s−1, respectively. Differences between these results and other measurements of reaction (1) are discussed. The relevance of reaction (1) to the formation of HC3N in interstellar clouds is also briefly assessed.


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