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Molecule formation in normal cloudsSome aspects of molecule formation in normal interstellar clouds, i.e., clouds having particle densities of less than 100 per cu cm, are discussed in light of recent studies. It is pointed out that, with their relatively large depletion parameter values (DPVs), CH clouds are 'young', whereas OH clouds have small DPVs and are 'old'. The theoretical reason for this is that OH, as a product of grain catalysis, persists over a much longer period of cloud evolution, whereas CH(+), CH, and CN, as products of gas-phase reaction, can be found only in 'young' clouds where depletion has not yet occurred. This may explain why OH has not been seen in radio observations of regions where CH(+), CH, and CN have been seen optically.
Document ID
19740054684
Acquisition Source
Legacy CDMS
Document Type
Other - Collected Works
Authors
Aannestad, P. A.
(California, University Berkeley, Calif.; NASA, Goddard Institute for Space Studies, New York, N.Y., United States)
Date Acquired
August 7, 2013
Publication Date
January 1, 1973
Subject Category
Physics, Atomic, Molecular, And Nuclear
Accession Number
74A37434
Distribution Limits
Public
Copyright
Other

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