High-temperature water–rock interactions and hydrothermal environments in the chondrite-like core of Enceladus

Yasuhito Sekine (), Takazo Shibuya, Frank Postberg, Hsiang-Wen Hsu, Katsuhiko Suzuki, Yuka Masaki, Tatsu Kuwatani, Megumi Mori, Peng K. Hong, Motoko Yoshizaki, Shogo Tachibana and Sin-iti Sirono
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Yasuhito Sekine: University of Tokyo
Takazo Shibuya: Laboratory of Ocean-Earth Life Evolution Research, Japan Agency for Marine-Earth Science and Technology
Frank Postberg: Institut für Geowissenschaften, Universität Heidelberg
Hsiang-Wen Hsu: Laboratory for Atmospheric and Space Physics, University of Colorado
Katsuhiko Suzuki: Research and Development Center for Submarine Resources / Project Team for Next-Generation Technology for Ocean Resources Exploration, Japan Agency for Marine-Earth Science and Technology
Yuka Masaki: Research and Development Center for Submarine Resources / Project Team for Next-Generation Technology for Ocean Resources Exploration, Japan Agency for Marine-Earth Science and Technology
Tatsu Kuwatani: Japan Agency for Marine-Earth Science and Technology
Megumi Mori: Hokkaido University
Peng K. Hong: The University Museum, University of Tokyo
Motoko Yoshizaki: Tokyo Institute of Technology
Shogo Tachibana: Hokkaido University
Sin-iti Sirono: Graduate School of Environmental Science, Nagoya University

Nature Communications, 2015, vol. 6, issue 1, 1-8

Abstract: Abstract It has been suggested that Saturn’s moon Enceladus possesses a subsurface ocean. The recent discovery of silica nanoparticles derived from Enceladus shows the presence of ongoing hydrothermal reactions in the interior. Here, we report results from detailed laboratory experiments to constrain the reaction conditions. To sustain the formation of silica nanoparticles, the composition of Enceladus’ core needs to be similar to that of carbonaceous chondrites. We show that the presence of hydrothermal reactions would be consistent with NH3- and CO2-rich plume compositions. We suggest that high reaction temperatures (>50 °C) are required to form silica nanoparticles whether Enceladus’ ocean is chemically open or closed to the icy crust. Such high temperatures imply either that Enceladus formed shortly after the formation of the solar system or that the current activity was triggered by a recent heating event. Under the required conditions, hydrogen production would proceed efficiently, which could provide chemical energy for chemoautotrophic life.

Date: 2015
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DOI: 10.1038/ncomms9604

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