49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2358.pdf CHARIOT TO THE MOONS OF MARS. D.A. Minton1, D. Spencer1, B. Horgan1, Z. Putnam2, J. Puig-Suari3, and P. Christensen4, 1Purdue University, West Lafayette, IN 47907, USA, (
[email protected]), 2University of Illinois Urbana-Champaign, Urbana Illinois 61801, 3Tyvak Corporation, Irvine, CA 92618, 4Arizona State University, Tempe, AZ 85281. Introduction: The origin of the two moons of spatial resolution and coverage to tie observed spectral Mars, Phobos and Deimos, remains a major unsolved variability to specific surface features and geologic pro- mystery in our understanding of planet and satellite for- cesses [15]. In addition, Deimos is virtually unstudied. mation. Existing observations of Phobos and Deimos A major distinguishing feature of the different origin are insufficient to determine which of the many pro- models for Phobos and Deimos is in the relationship be- posed models for their origin and modification history tween the two bodies. At one extreme, the Intact Cap- is correct. Proposed origin models include capture of as- ture model holds that the satellites are wholly unrelated teroids, contemporaneous formation with Mars, and for- to each other, while Protosatellite Disk Hypothesis mation from an impact-generated debris disk. The lack models suggest varying degrees of commonality in the of a definitive origin model also has major implications starting material and post-formation processing of satel- for human exploration, as the amount of extractable re- lites. To address this major knowledge gap, the Chariot sources needed to aid in human exploration of Mars is mission will conduct a high-resolution observing cam- tied to the moons’ formation and evolution.