Temperature and pressure determinations in the Venus atmosphere by means of high-resolution spectra from 1 to 2.5 μm

Karl E. Dierenfeldt, Uwe - Fink, Harold P. Larson

Research output: Contribution to journalArticle

Abstract

Twenty-one bands of CO2 and the 2-0 band of CO were analyzed for best temperature and pressure fits from Venus spectra obtained with the "Connes" interferometer at the Steward Observatory 2.25-m telescope during the spring of 1971. An average temperature of 241 ± 7°K, an effective pressure of 0.12 ± 0.06 atm, and an average two-way transmission abundance of 3 km-amagat were determined. No difference in temperature or pressure between hot bands, a double hot band, and regular bands was found. Our results were compared to model calculations for a reflecting layer and scattering atmosphere. The results indicate that, most likely, spectroscopic line formation occurs in a relatively clear space above a scattering cloud layer with a reasonably well-defined upper boundary.

Original languageEnglish (US)
Pages (from-to)11-24
Number of pages14
JournalIcarus
Volume31
Issue number1
DOIs
StatePublished - 1977

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Venus atmosphere
Venus
atmosphere
high resolution
scattering
temperature
interferometer
observatory
Venus (planet)
observatories
interferometers
telescopes
atmospheres

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Temperature and pressure determinations in the Venus atmosphere by means of high-resolution spectra from 1 to 2.5 μm. / Dierenfeldt, Karl E.; Fink, Uwe -; Larson, Harold P.

In: Icarus, Vol. 31, No. 1, 1977, p. 11-24.

Research output: Contribution to journalArticle

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AB - Twenty-one bands of CO2 and the 2-0 band of CO were analyzed for best temperature and pressure fits from Venus spectra obtained with the "Connes" interferometer at the Steward Observatory 2.25-m telescope during the spring of 1971. An average temperature of 241 ± 7°K, an effective pressure of 0.12 ± 0.06 atm, and an average two-way transmission abundance of 3 km-amagat were determined. No difference in temperature or pressure between hot bands, a double hot band, and regular bands was found. Our results were compared to model calculations for a reflecting layer and scattering atmosphere. The results indicate that, most likely, spectroscopic line formation occurs in a relatively clear space above a scattering cloud layer with a reasonably well-defined upper boundary.

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