This paper points out the difficulties in distinguishing between an upper and lower Venusian atmosphere and notes the lack of basic data on surface pressure and temperature, temperature gradients, gaseous and particulate composition, large- and small-scale air motion, and the nature of the planet's surface at the bottom of the atmosphere. The wide variation of recent surface pressure estimates, ranging between 3 and 1000 atmospheres, is displayed graphically. The paper was prepared for presentation at the Conference on the Atmospheres of Mars and Venus, Tucson, Arizona, Feburary 28, 1967. 9 pp.
This report is part of the RAND Corporation Paper series. The paper was a product of the RAND Corporation from 1948 to 2003 that captured speeches, memorials, and derivative research, usually prepared on authors' own time and meant to be the scholarly or scientific contribution of individual authors to their professional fields. Papers were less formal than reports and did not require rigorous peer review.
This document and trademark(s) contained herein are protected by law. This representation of RAND intellectual property is provided for noncommercial use only. Unauthorized posting of this publication online is prohibited; linking directly to this product page is encouraged. Permission is required from RAND to reproduce, or reuse in another form, any of its research documents for commercial purposes. For information on reprint and reuse permissions, please visit www.rand.org/pubs/permissions.
The RAND Corporation is a nonprofit institution that helps improve policy and decisionmaking through research and analysis. RAND's publications do not necessarily reflect the opinions of its research clients and sponsors.