Ambient and cold‐temperature infrared spectra and XRD patterns of ammoniated phyllosilicates and carbonaceous chondrite meteorites relevant to Ceres and other solar system bodies

1,2Bethany L. Ehlmann, 2Robert Hodyss, 3Thomas F. Bristow, 1George R. Rossman, 4,5Eleonora Ammannito M., 6Cristina De Sanctis, 5Carol A. Raymond
Meteoritics & Planetary Science (in Press) Link to Article []
1Division of Geological & Planetary Sciences, California Institute of Technology, Pasadena, California, USA
2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
3Exobiology Branch, NASA Ames Research Center, Moffett Field, California, USA
4Department of Earth Planetary and Space Sciences, University of California, Los Angeles, California, USA
5Italian Space Agency (ASI), , Rome, Italy
6Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, , Rome, Italy
Published by arrangement with John Wiley & Sons

Mg‐phyllosilicate‐bearing, dark surface materials on the dwarf planet Ceres have NH4‐bearing materials, indicated by a distinctive 3.06 μm absorption feature. To constrain the identity of the Ceres NH4‐carrier phase(s), we ammoniated ground particulates of candidate materials to compare their spectral properties to infrared data acquired by Dawn’s Visible and Infrared (VIR) imaging spectrometer. We treated Mg‐, Fe‐, and Al‐smectite clay minerals; Mg‐serpentines; Mg‐chlorite; and a suite of carbonaceous meteorites with NH4‐acetate to exchange ammonium. Serpentines and chlorites showed no evidence for ammoniation, as expected due to their lack of exchangeable interlayer sites. Most smectites showed evidence for ammoniation by incorporation of NH4+ into their interlayers, resulting in the appearance of absorptions from 3.02 to 3.08 μm. Meteorite samples tested had weak absorptions between 3.0 and 3.1 μm but showed little clear evidence for enhancement upon ammoniation, likely due to the high proportion of serpentine and other minerals relative to expandable smectite phases or to NH4+ complexing with organics or other constituents. The wavelength position of the smectite NH4 absorption showed no variation between IR spectra acquired under dry‐air purge at 25 °C and under vacuum at 25 °C to −180 °C. Collectively, data from the smectite samples show that the precise center wavelength of the characteristic ~3.05 μm v3 absorption in NH4 is variable and is likely related to the degree of hydrogen bonding of NH4‐H2O complexes. Comparison with Dawn VIR spectra indicates that the hypothesis of Mg‐saponite as the ammonium carrier phase is the simplest explanation for observed data, and that Ceres dark materials may be like Cold Bokkeveld or Tagish Lake but with proportionally more Mg‐smectite.


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