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Models for the Venus atmosphere and ionosphere are presented and compared with data obtained in the S-band occultation experiment on Mariner 5. Good agreement is found between model and experiment if the Venus atmosphere is composed of essentially pure CO2. An upper limit of about 10% is derived for the N2 mixing rate. It is argued that atomic oxygen is a minor constituent in the upper atmosphere of Venus.
Models for the Venus atmosphere and ionosphere are presented and compared with data obtained in the S-band occultation experiment on Mariner 5. Good agreement is found between model and experiment if the Venus atmosphere is composed of essentially pure CO2. An upper limit of about 10% is derived for the N2 mixing rate. It is argued that atomic oxygen is a minor constituent in the upper atmosphere of Venus.
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