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In-situ Venus Missions The Need for In-Situ missions: Despite years of exploration, major questions remain: • What is the precise chemical composition of the atmosphere and how does it vary with location and altitude? • When and How did the Greenhouse effect occur on Venus • How did the atmosphere of Venus form and evolve? • What are the morphology, chemical make-up, and variability of the Venusian clouds and their impact on the climate? • What are the processes controlling the atmospheric super-rotation? • What are the processes governing Venus seismicity and its interior structure? • How have the interior, surface, and atmosphere interacted as a coupled system over time? Fig. 1 Venus temperature/pressure vs. altitude 22 The Problem • Hostile environment of high temperature and pressure (465°C and 92 atm of CO2) makes surface and low-altitude missions challenging. • Cloud opacity limits orbital/balloon observations • Conventional power sources, PV or RTG may not be applicable. New power technologies desired to enable missions Battery Options Non-Existent Fig. 1 Venus temperature/pressure vs. altitude.PDF Image | NASA Fuel Cell and Hydrogen Activities
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