Surface Environment of Phobos and Phobos Simulant UTPS
Hideaki Miyamoto ( [email protected] ) University of Tokyo https://orcid.org/0000-0001-8013-6124 Takafumi Niihara University of Tokyo Graduate School of Engineering School of Engineering: Tokyo Daigaku Daigakuin Kogakukei Kenkyuka Kogakubu Koji Wada Chiba Institute of Technology: Chiba Kogyo Daigaku Kazunori Ogawa Japan Aerospace Exploration Agency Hiroki Senshu Chiba Institute of Technology: Chiba Kogyo Daigaku Patrick Michel Observatoire de la Côte d'Azur: Observatoire de la Cote d'Azur Hiroshi Kikuchi JAXA Ryodo Hemmi University of Tokyo Graduate School of Engineering School of Engineering: Tokyo Daigaku Daigakuin Kogakukei Kenkyuka Kogakubu Tomoki Nakamura Tohoku University: Tohoku Daigaku Akiko M Nakamura Kobe University Naoyuki Hirata Kobe University Sho Sasaki Osaka University Erik Asphaug University of Arizona Dan T. Britt University of Central Florida Paul A. Abell NASA Lyndon B Johnson Space Center: NASA Johnson Space Center Ronald-Louis Ballouz
Page 1/10 University of Arizona Olivier S. Barnouin The Johns Hopkins University Nicola Barsei University of Surrey Maria A. Barucci Observatoire de Paris Jens Biele German Aerospace Center Matthias Grott German Aerospace Center Hideitsu Hino The institute of Statistical Mathematics Peng K. Hong Chiba Institute of Technology: Chiba Kogyo Daigaku Takane Imada JAXA Shingo Kameda Rikkyo University: Rikkyo Daigaku Makito Kobayashi University of Tokyo Guy Libourel Observatoire de la Côte d'Azur: Observatoire de la Cote d'Azur Katsuro Mogi University of Tokyo: Tokyo Daigaku Naomi Murdoch ISAE-SUPAERO Yuki Nishio University of Tokyo: Tokyo Daigaku Shogo Okamoto University of Tokyo: Tokyo Daigaku Yuichiro Ota University of Tokyo: Tokyo Daigaku Masatsugu Otsuki JAXA Katharina A. Otto German Aerospace Center Naoya Sakaani Rikkyo University: Rikkyo Daigaku
Page 2/10 Yuta Shimizu University of Tokyo: Tokyo Daigaku Tomohiro Takemura University of Tokyo: Tokyo Daigaku Naoki Terada Tohoku University Masafumi Tsukamoto University of Tokyo: Tokyo Daigaku Tomohiro Usui JAXA Konrad Willner German Aerospace Center Institute of Planetary Research: Deutsches Zentrum fur Luft- und Raumfahrt DLR Institut fur Planetenforschung
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Keywords: MMX, Phobos, Deimos, Surface environment, Simulant
Posted Date: January 20th, 2021
DOI: https://doi.org/10.21203/rs.3.rs-150345/v1
License: This work is licensed under a Creative Commons Attribution 4.0 International License. Read Full License
Page 3/10 Abstract
The Martian Moons eXploration (MMX) mission will study the Martian moons Phobos and Deimos, Mars, and their environments. The mission scenario includes both landing on the surface of Phobos to collect samples and deploying a small rover for in-situ observations. Engineering safeties and scientifc planning for these operations require appropriate evaluations of the surface environment of Phobos. Thus, the mission team organized the Landing Operation Working Team (LOWT) and Surface Science and Geology Sub-Science Team (SSG-SST), whose view of the Phobos environment is summarized in this paper. While orbital and large-scale characteristics of Phobos are relatively well known, characteristics of the surface regolith, including the particle size-distributions, the packing density, and the mechanical properties, are difcult to constrain. Therefore, we developed several types of simulated soil materials (simulant), such as UTPS-TB (University of Tokyo Phobos Simulant, Tagish-lake based), UTPS-IB (Impact-hypothesis based), and UTPS-S (Simpler version) for engineering and scientifc evaluation experiments.
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Figures
Figure 1
Page 4/10 (a) Phobos’ 2D map, color-coded with respect to dynamic surface slope. Tidal effect is included; (b) Binarized slope map at 10 degrees; (c) Frequency distributions of dynamic surface slopes (bars) and its cumulative plot (red line).
Figure 2
Correlation-based mutual distances of 556 meteorites, 259 asteroids, and Phobos’s blue and red units visualized by t-SNE approach, which shows the correlations between C-type asteroids and C-type meteorites. Colors represent types of asteroids and meteorites as denoted in the bottom. Inset is the closeup of the upper middle part of the plot, which shows both the red and the blue units of Phobos is best matched with the Tagish lake meteorite, which is surrounded by the greenish rectangle.
Page 5/10 Figure 3
Estimated surface and subsurface structure.
Page 6/10 Figure 4
Conceptual model of particle size distributions of regolith on Phobos
Page 7/10 Figure 5
Optical and backscattered electron images of UTPS-TB (A, B,C) simulant and Tagish Lake meteorite (D,E,F). UTPS-TB simulate petrographical signature: Phenocrysts of silicate and opaque minerals are embedded in a loosely jammed fne grained (<20 µm) serpentine matrix. UTPS-TB simulates mineral abundance and visible and near-infrared refectance of Tagish Lake meteorite.
Figure 6
Refectance spectra for UTPS-TB, -IB, and the Murchison meteorite compared with Phobos I/F spectra (red and blue units; data extracted from Fig. 4 of Fraeman et al., 2012).
Page 8/10 Figure 7
Simulated surface of Phobos using UTPS-TB with the observed crater size-frequency distributions and incidence angles of 70 degrees (a) and 10 degrees (b). Close-up views of Phobos’ surface (c, d; Parts of MGS Mars Orbiter Camera image 55103).
Supplementary Files Page 9/10 This is a list of supplementary fles associated with this preprint. Click to download.
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