Cover Page/Proposal Summary
Date Due: 5/3/99
NASA PROCEDURE FOR HANDLING PROPOSALS
This proposal shall be used and disclosed for evaluation purposes only, and
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on this proposal shall also be strictly complied with. Disclosure
proposal for any reason outside the Government evaluation purposes
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|Proposal Type: New
|Proposal Category: Laboratory|
|Major Equipment Proposal?
|Do you intend to submit an Education/Public Outreach (E/PO)
the nightglow of Venus|
|O2(a,b,c) in the nightglow of
|Dr. Tom G.
Molecular Physics Lab
Menlo Park, CA 94025-3493
Phone: 650-859-2764 Fax:
|Sci Co-I ||Dr. Richard A.
We propose to determine the yields into three O2
electronically-excited states -
denoted O2(a), O2(b), and O2(c) -
following O2 photoexcitation close to the
dissociation limit, in O2
and CO2 buffers. CO2 is the environment in which the
is generated, and two of the above states, O2(a,v=0) and
are strong Venus emitters, while O2(a,v=0) and O2(b,v=0) are strong
emitters in the terrestrial atmosphere. We argue, based on our recent
that photoexcitation of O2 to levels near the dissociation
limit is equivalent,
in the sense of the evolution of the system, to
the atom recombination process.
A number of investigations, based on observations in both
atmospheres, have led
to problems of interpretation of emission
intensities. Particularly in the case
of the O2(a-X) 0-0 Infrared
Atmospheric Band at Venus, it has been suggested
that the emission
intensity is much greater than expected. From the yields we
determine from laboratory measurements as well as the loss rate
coefficients of the O2(c,v=0) level that we propose to measure, we
definitively show the major pathways by which O-atom
which will then guide interpretation of past
and future observations of
planetary oxygen atmospheres.