Anomalously porous boulders on (162173) Ryugu as primordial materials from its parent body

Sakatani, N.; Tanaka, S.; Okada, T.; Fukuhara, T.; Riu, L.; Sugita, S.; Honda, R.; Morota, T.; Kameda, S.; Yokota, Y.; Tatsumi, E.; Yumoto, K.; Hirata, N.; Miura, A.; Kouyama, T.; Senshu, H.; Shimaki, Y.; Arai, T.; Takita, J.; Demura, H.; Sekiguchi, T.; Müller, T. G.; Hagermann, A.; Biele, J.; Grott, M.; Hamm, M.; Delbo, M.; Neumann, W.; Taguchi, M.; Ogawa, Y.; Matsunaga, T.; Wada, T.; Hasegawa, S.; Helbert, J.; Hirata, N.; Noguchi, R.; Yamada, M.; Suzuki, H.; Honda, C.; Ogawa, K.; Hayakawa, M.; Yoshioka, K.; Matsuoka, M.; Cho, Y.; Sawada, H.; Kitazato, K.; Iwata, T.; Abe, M.; Ohtake, M.; Matsuura, S.; Matsumoto, K.; Noda, H.; Ishihara, Y.; Yamamoto, K.; Higuchi, A.; Namiki, N.; Ono, G.; Saiki, T.; Imamura, H.; Takagi, Y.; Yano, H.; Shirai, K.; Okamoto, C.; Nakazawa, S.; Iijima, Y.; Arakawa, M.; Wada, K.; Kadono, T.; Ishibashi, K.; Terui, F.; Kikuchi, S.; Yamaguchi, T.; Ogawa, N.; Mimasu, Y.; Yoshikawa, K.; Takahashi, T.; Takei, Y.; Fujii, A.; Takeuchi, H.; Yamamoto, Y.; Hirose, C.; Hosoda, S.; Mori, O.; Shimada, T.; Soldini, S.; Tsukizaki, R.; Ozaki, M.; Tachibana, S.; Ikeda, H.; Ishiguro, M.; Yabuta, H.; Yoshikawa, M.; Watanabe, S.; Tsuda, Y.
Bibliographical reference

Nature Astronomy

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Planetesimals—the initial stage of the planetary formation process—are considered to be initially very porous aggregates of dusts1,2, and subsequent thermal and compaction processes reduce their porosity3. The Hayabusa2 spacecraft found that boulders on the surface of asteroid (162173) Ryugu have an average porosity of 30-50% (refs. 4-6), higher than meteorites but lower than cometary nuclei7, which are considered to be remnants of the original planetesimals8. Here, using high-resolution thermal and optical imaging of Ryugu's surface, we discovered, on the floor of fresh small craters (<20 m in diameter), boulders with reflectance (~0.015) lower than the Ryugu average6 and porosity >70%, which is as high as in cometary bodies. The artificial crater formed by Hayabusa2's impact experiment9 is similar to these craters in size but does not have such high-porosity boulders. Thus, we argue that the observed high porosity is intrinsic and not created by subsequent impact comminution and/or cracking. We propose that these boulders are the least processed material on Ryugu and represent remnants of porous planetesimals that did not undergo a high degree of heating and compaction3. Our multi-instrumental analysis suggests that fragments of the highly porous boulders are mixed within the surface regolith globally, implying that they might be captured within collected samples by touch-down operations10,11.
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Minor Bodies of the Solar System

This project studies the physical and compositional properties of the so-called minor bodies of the Solar System, that includes asteroids, icy objects, and comets. Of special interest are the trans-neptunian objects (TNOs), including those considered the most distant objects detected so far (Extreme-TNOs or ETNOs); the comets and the comet-asteroid

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