Date of Graduation

5-2011

Document Type

Thesis

Degree Name

Bachelor of Science in Mechanical Engineering

Degree Level

Undergraduate

Department

Mechanical Engineering

Advisor/Mentor

Roe, Larry A.

Committee Member/Reader

Chevrier, Vincent

Abstract

While the atmospheric chemical composition of the Venusian atmosphere has been characterized at length by probes and ground-based equipment, the surface mineralogy of Venus is not yet well understood. The extremely thick atmosphere of Venus shields the surface from direct observation. While radar imaging of the surface reveals surface morphology, surface composition is difficult to characterize at a distance. Observation is also difficult due to the intense temperature (approximately 480°C) and pressure (approximately 90 atm) found on the surface. This has prompted NASA and other institutions around the world to begin planning for new missions to land on the surface of Venus to better understand its composition, structure, and other features.
As a “sister” planet to Earth in terms of size and mass, Venus provides an interesting object of study for comparison (Landis, 2006). Though similar in bulk, Venus’s surface is dramatically different than Earth’s. Instead of liquid water and temperate climates, Venus is covered by a thick cloud layer and scorching winds. Even though it is close to being in Sol’s habitable zone, the surface is not remotely conducive to life. Earlier in the planet’s history, though, it could have been in the habitable zone, but obviously surface conditions have dramatically changed since then. Understanding more about the surface chemistry and mineralogy of the planet will allow scientists to better understand the planet’s history. By understanding Venus’s history, scientists can better understand what caused this dramatic transformation. This will be essential to preventing the same transformations on Earth.
Venus’s atmosphere is the most notable and most studied feature of the planet. The hot, thick mass of swirling gases is not found on any other terrestrial planet. Although scientifically interesting itself, this shroud has made effective study of the planet’s surface difficult. Only limited direct observation is available from the Soviet Venera missions and American Pioneer probes. This makes future landers particularly attractive for extensive surface study.
The destructive conditions found at the surface make direct exploration difficult, though. Landers must be structurally sound enough to survive the intense pressure, and electronics must be able to perform at temperatures hot enough to melt the solder that typically holds them together. Engineering such a craft is difficult, and obtaining useful scientific results to justify the mission is even more so. Without a proper method of analysis and mineralogical characterization, missions to the surface will not be successful. Infrared spectroscopy holds promise to meet the demands of the mission while producing valuable scientific results. As a low-weight, low-power device, an infrared spectrometer would allow scientists to characterize the minerals found of the surface of the planet much more effectively than previously observed. More study is necessary to characterize the response of both minerals and equipment to the high temperatures that will be seen on an actual mission. Most importantly, spectra could change due to temperature-induced changes in crystallization, composition, or other physical characteristics, which will be the focus of this study.

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