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Subsurface Chemistry of the Imbrium Basin Inferred from Clementine UVVIS Spectroscopy

Earth, Planets and Space volume 58, pages 1499–1510 (2006)Cite this article

Abstract

Since ejecta around an impact crater is excavated from a depth, its mineralogy and chemistry will provide us with information on the composition of the pre-impact subsurface. The depth from which crater ejecta were excavated was determined from laboratory experiments, field studies, and a simplified quantitative model (Z-model and the scaling law of ejection velocity). Based on the results of these studies, it is believed that surface material of an ejecta blanket between 1.1 and 1.5 radii from the crater was excavated from a depth of 0.13 to 0.15 radii. The following results were obtained from combining the surface and subsurface basalt distributions with crater-counting ages for the mare basalt, we obtained the following results: (1) The averages of TiO2 and FeO increased with time from the Imbrian to the Eratosthenian periods, which is represented by a continuous trend curve on the TiO2-FeO graph: (2) volcanic activities in Mare Imbrium drastically decreased and basalts changed from a low-Ti to high-Ti content around the transition of the Imbrian to Eratosthenian period: (3) basalts with less than 3 wt% TiO2 erupted in succession mainly in the Imbrian period.

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Affiliations

  1. SELENE project team, ISAS, JAXA, Sengen, Tsukuba, Ibaraki, 305-8505, Japan

    Hisashi Otake

  2. Division of Planetary Science, ISAS, JAXA, Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan

    Hitoshi Mizutani

  3. Newton Press Inc., Nishi-Shinjuku, Shinjuku-ku, Tokyo, 163-0207, Japan

    Hitoshi Mizutani

Authors
  1. Hisashi Otake
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  2. Hitoshi Mizutani
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Correspondence to Hisashi Otake.

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Otake, H., Mizutani, H. Subsurface Chemistry of the Imbrium Basin Inferred from Clementine UVVIS Spectroscopy. Earth Planet Sp 58, 1499–1510 (2006). https://doi.org/10.1186/BF03352649

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Key words

  • Imbrium basin
  • subsurface
  • ejecta
  • age
  • volcanism