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@ARTICLE{Lee:281812,
      author       = {Lee, M. R. and MacLaren, I. and Andersson, S. M. L. and
                      Kovács, A. and Tomkinson, T. and Mark, D. F. and Smith, C.
                      L.},
      title        = {{O}pal-{A} in the {N}akhla meteorite: {A} tracer of
                      ephemeral liquid water in the {A}mazonian crust of {M}ars},
      journal      = {Meteoritics $\&$ planetary science},
      volume       = {50},
      number       = {8},
      issn         = {1086-9379},
      address      = {Hoboken, NJ},
      publisher    = {Wiley-Blackwell},
      reportid     = {FZJ-2016-01479},
      pages        = {1362 - 1377},
      year         = {2015},
      abstract     = {The nakhlite meteorites are clinopyroxenites that are
                      derived from a ~1300 million year old sill or lava flow on
                      Mars. Most members of the group contain veins of iddingsite
                      whose main component is a fine-grained and hydrous Fe- and
                      Mg-rich silicate. Siderite is present in the majority of
                      veins, where it straddles or cross-cuts the Fe-Mg silicate.
                      This carbonate also contains patches of ferric
                      (oxy)hydroxide. Despite 40 years of investigation, the
                      mineralogy and origins of the Fe-Mg silicate is poorly
                      understood, as is the paragenesis of the iddingsite veins.
                      Nanometer-scale analysis of Fe-Mg silicate in the Nakhla
                      meteorite by electron and X-ray imaging and spectroscopy
                      reveals that its principal constituents are nanoparticles of
                      opal-A. This hydrous and amorphous phase precipitated from
                      acidic solutions that had become supersaturated with respect
                      to silica by dissolution of olivine. Each opal-A
                      nanoparticle is enclosed within a ferrihydrite shell that
                      formed by oxidation of iron that had also been liberated
                      from the olivine. Siderite crystallized subsequently and
                      from solutions that were alkaline and reducing, and replaced
                      both the nanoparticles and olivine. The fluids that formed
                      both the opal-A/ferrihydrite and the siderite were sourced
                      from one or more reservoirs in contact with the Martian
                      atmosphere. The last event recorded by the veins was
                      alteration of the carbonate to a ferric (oxy)hydroxide that
                      probably took place on Mars, although a terrestrial origin
                      remains possible. These results support findings from
                      orbiter- and rover-based spectroscopy that opaline silica
                      was a common product of aqueous alteration of the Martian
                      crust.},
      cin          = {PGI-5},
      ddc          = {520},
      cid          = {I:(DE-Juel1)PGI-5-20110106},
      pnm          = {143 - Controlling Configuration-Based Phenomena (POF3-143)},
      pid          = {G:(DE-HGF)POF3-143},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:000359356900003},
      doi          = {10.1111/maps.12471},
      url          = {https://juser.fz-juelich.de/record/281812},
}