Reactions of CmHϩn ions with O atoms
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J. Chem. Phys., Vol. 112, No. 11, 15 March 2000
the reactions of those CmHnϩ ions that are unreactive with H2
but reactive with O need to be re-examined in the models.
Included in this category are the reactions with C2Hϩ4 , C3H3ϩ,
C4Hϩ2 , c-C6Hϩ5 , and c-C6Hϩ6 .
Finally we note that in diffuse interstellar clouds, atom
densities are enhanced29 and ion atom reactions may have a
different role than in dense clouds.
bon ion reactions with atomic oxygen is the presence of mul-
tiple reaction channels that were found in all reactive
encounters. In a similar study of seventeen hydrocarbons
with atomic nitrogen,11 seven had reactions with rate coeffi-
cients kϾ1ϫ10Ϫ10 cm3 sϪ1, and therefore the fraction of re-
active encounters was slightly greater for atomic oxygen
with eight out of thirteen having kу1ϫ10Ϫ10 cm3 sϪ1. Fur-
ther, the reaction complexity was greater for reactions with O
atoms. Generally, ions unreactive with N atoms were also
unreactive with O atoms ͑e.g., C2Hϩ5 , c-C3H3ϩ, ac-C3H5ϩ,
C4Hϩ3 , and ac-C6Hϩ5 ). Another aspect of the comparison is
that whereas CmHϩn ion N atom reactions had a propensity to
form HCN ion or neutral products, O atoms favored HCO
ion products for mϽ3, but CO neutral products for mу3.
Other characteristics common to both investigations were the
number of reactions that apparently violate spin conserva-
tion. This observation has been commented on previously by
Ferguson and colleagues.21,25
ACKNOWLEDGMENT
We thank the Marsden fund for financial support of this
work.
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The absence of any reaction with O atoms by four hy-
drocarbon ions was not because of a lack of exothermic
product channels. For example, although C2Hϩ5 did not react
with atomic oxygen, the product channel to HCOϩϩCH4 is
6 V. Le Page, Y. Keheyan, V. M. Bierbaum, and T. P. Snow, J. Am. Chem.
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7 G. B. I. Scott, D. A. Fairley, D. B. Milligan, C. G. Freeman, and M. J.
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exothermic by 399 kJ molϪ1
,
8 M. J. McEwan, in Advances in Gas Phase Ion Chemistry, edited by N. G.
Adams and L. M. Babcock ͑JAI, Greenwich, CT, 1992͒, Vol. 1, p. 1.
9 P. D. Goldan, A. L. Schmeltekopf, F. C. Fehsenfeld, H. I. Schiff, and E. E.
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C2Hϩ5 ϩOyHCOϩϩCH4.
͑13͒
Presumably the barriers on the potential surface are too high
for the extensive rearrangement required. An alternative to a
bimolecular reaction is a termolecular association reactions,
i.e.,
10 G. B. I. Scott, D. A. Fairley, C. G. Freeman, and M. J. McEwan, J. Chem.
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11 G. B. I. Scott, D. A. Fairley, C. G. Freeman, M. J. McEwan, and V. G.
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12 Webbook, W. G. Mallard, Gen. Ed. ͑NIST, Gaithersburg, MD, 1998͒.
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186Õ187, 253 ͑1999͒.
C2Hϩ5 ϩOϩMyC2H5OϩϩM.
͑14͒
Although reaction ͑14͒ is exothermic by 568 kJ molϪ1 for the
formation of CH3CHOHϩ, it is not observed. The lack of
association reactions for small CmHϩn –atom reactions is a
consequence of the short lifetime of the intermediate because
of the energy carried into the complex by the atom. O atom
association may be a more important outcome for larger
CmHϩn ions where the excess energy in the complex can be
accommodated by the large number of energy modes. In-
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et al.6 for the C10Hϩ8 ϩO reaction.
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Atomic oxygen can be a significant component of inter-
stellar clouds26 and in dark clouds the aggregate amount of
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Orion compact ridge near the luminous infrared source
IRc2.28 Bettens and Brown27 have considered participation
by hydrogen ion–O atom reactions in interstellar cloud
chemistry and concluded that the influence of these reactions
on the chemistry of the clouds was small whereas neutral–O
atom chemistry may play a much more significant role. Since
their study, however, more data have become available and
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28 T. J. Millar, E. Herbst, and S. B. Charnley, Astrophys. J. 369, 147 ͑1991͒.
29
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