Associate for Education and Public Outreach

田畑 陽久

タバタ ハルヒサ  (Haruhisa Tabata)

基本情報

所属
国立研究開発法人宇宙航空研究開発機構 宇宙科学研究所 宇宙航空プロジェクト研究員
学位
博士(理学)(2022年3月 東京大学)

研究者番号
70962372
ORCID ID
 https://orcid.org/0000-0002-5653-5982
J-GLOBAL ID
202301015883174793
researchmap会員ID
R000047023

研究キーワード

 3

論文

 7
  • Yuki Uchida, Kosei Toyokawa, Tomohiro Usui, Yudai Suzuki, Haruhisa Tabata
    Progress in Earth and Planetary Science 12(1) 2025年8月19日  査読有り
    Abstract Phobos always keeps the same side facing its host planet like Earth’s Moon, making it a key comparative target for studying the coevolution of planet–satellite systems. The heterogeneity of satellite surface evolution under a host planet’s gravity is crucial for understanding the evolution of such systems. This study examines the crater size–frequency distribution (CSFD) across four equatorial regions of Phobos—leading, near, trailing, and far sides—to investigate surface evolution heterogeneities linked to resurfacing and orbital dynamics following the formation of its largest crater, Stickney. We focus on the crater size indicating the number of craters lower than expected from the production function (PF) model. We also estimate the crater erasure scale due to the ejecta blanket and assess deviations in the size–frequency distribution (SFD) of impactors from the PF model. This study shows three main conclusions about surface heterogeneity in Phobos’ CSFD and ejecta blanket thickness. (1) The leading side experienced significant crater erasure, likely due to the thickest ejecta blanket from the Stickney impact. (2) The density of craters larger than $$\sim$$ 1.5 km reflects pre-Stickney conditions, whereas the densities of craters measuring 0.8–1.5 km and 400–800 m in diameter reflect post-Stickney surface evolution. (3) Crater number density on the near side was consistently lower than on the far side, likely due to planetary screening. This reduction in crater formation on the near side is particularly attributed to its proximity to Mars. Our results suggest that the leading side experienced the greatest deposition of the ejecta blanket on Phobos. This deposition likely occurred immediately after Stickney’s formation, followed by global resurfacing facilitated by Phobos’ post-Stickney impact spin. One possible explanation for the scarcity of craters smaller than 800 m is that later-arriving, low-energy impacts erased smaller preexisting craters while leaving larger ones comparatively well preserved, leading to a net reduction in their population.
  • K. Yumoto, Y. Cho, J. A. Ogura, S. Kameda, T. Niihara, T. Nakaoka, R. Kanemaru, H. Nagaoka, H. Tabata, Y. Nakauchi, M. Ohtake, H. Ueda, S. Kasahara, T. Morota, S. Sugita
    Spectrochimica Acta - Part B Atomic Spectroscopy 221 2024年11月  査読有り
  • Haruhisa Tabata, Yasuhito Sekine, Kazumi Ozaki
    Geochimica et Cosmochimica Acta 381 97-115 2024年9月15日  査読有り筆頭著者
  • Yuichiro Cho, Yayoi N. Miura, Hikaru Hyuga, Kenta Shimokoshi, Kazuo Yoshioka, Hiroyuki Kurokawa, Hidenori Kumagai, Naoyoshi Iwata, Satoshi Kasahara, Haruhisa Tabata, Mari Aida, Yoshifumi Saito, Seiji Sugita
    The Planetary Science Journal 2024年8月1日  査読有り
  • Haruhisa TABATA, Yuichiro CHO, Kazuo YOSHIOKA, Mari AIDA, Kasumi YOGATA, Masato HAYASHIDA, Tsuyoshi KANDA, Yui KAWAKAMI, Junya TOEDA, Shin-ichiro SATO, Mitsuru IMAIZUMI
    JAXA Research and Development Report 23 2024年2月14日  査読有り筆頭著者

担当経験のある科目(授業)

 1

共同研究・競争的資金等の研究課題

 3