Laboratory spectroscopic detection of hydration in pristine lunar regolith

Matthew R.M. Izawa; Edward A. Cloutis; Daniel M. Applin; Michael A. Craig; Paul Mann; Matthew Cuddy

doi:10.1016/j.epsl.2014.01.007

Laboratory spectroscopic detection of hydration in pristine lunar regolith

Matthew R.M. Izawa, Edward A. Cloutis, Daniel M. Applin, Michael A. Craig, Paul Mann, Matthew Cuddy

Research output: Contribution to journal › Article › peer-review

7 Citations (Scopus)

Abstract

Reflectance spectroscopy of Apollo lunar soil samples curated in an air- and water-free, sealed environment since recovery and return to Earth has been carried out under water-, oxygen-, CO₂- and organic-controlled conditions. Spectra of these pristine samples contain features near 3 μm wavelength similar to those observed from the lunar surface by the Chandrayaan-1 Moon Mineralogy Mapper (M³), Cassini Visual and Infrared Mapping Spectrometer (VIMS), and Deep Impact Extrasolar Planet Observation and Deep Impact Extended Investigation (EPOXI) High-Resolution Instrument (HRI) instruments. Spectral feature characteristics and inferred OH/H₂O concentrations are within the range of those observed by spacecraft instruments. These findings confirm that the 3 μm feature from the lunar surface results from the presence of hydration in the form of bound OH and H₂O. Implantation of solar wind H⁺ appears to be the most plausible formation mechanism for most of the observed lunar OH and H₂O.

Original language	English
Pages (from-to)	157-164
Number of pages	8
Journal	Earth and Planetary Science Letters
Volume	390
DOIs	https://doi.org/10.1016/j.epsl.2014.01.007
Publication status	Published - Mar 15 2014
Externally published	Yes

Keywords

Apollo samples
Lunar hydration
Lunar regolith
Reflectance spectroscopy

ASJC Scopus subject areas

Geophysics
Geochemistry and Petrology
Earth and Planetary Sciences (miscellaneous)
Space and Planetary Science

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10.1016/j.epsl.2014.01.007

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title = "Laboratory spectroscopic detection of hydration in pristine lunar regolith",

abstract = "Reflectance spectroscopy of Apollo lunar soil samples curated in an air- and water-free, sealed environment since recovery and return to Earth has been carried out under water-, oxygen-, CO2- and organic-controlled conditions. Spectra of these pristine samples contain features near 3 μm wavelength similar to those observed from the lunar surface by the Chandrayaan-1 Moon Mineralogy Mapper (M3), Cassini Visual and Infrared Mapping Spectrometer (VIMS), and Deep Impact Extrasolar Planet Observation and Deep Impact Extended Investigation (EPOXI) High-Resolution Instrument (HRI) instruments. Spectral feature characteristics and inferred OH/H2O concentrations are within the range of those observed by spacecraft instruments. These findings confirm that the 3 μm feature from the lunar surface results from the presence of hydration in the form of bound OH and H2O. Implantation of solar wind H+ appears to be the most plausible formation mechanism for most of the observed lunar OH and H2O.",

keywords = "Apollo samples, Lunar hydration, Lunar regolith, Reflectance spectroscopy",

author = "Izawa, {Matthew R.M.} and Cloutis, {Edward A.} and Applin, {Daniel M.} and Craig, {Michael A.} and Paul Mann and Matthew Cuddy",

note = "Funding Information: M.R.M.I. gratefully acknowledges funding from the NSERC CREATE Canadian Astrobiology Training Program and the Mineralogical Association of Canada . The University of Winnipeg's HOSERLab was established with funding from the Canada Foundation for Innovation , the Manitoba Research Innovations Fund and the Canadian Space Agency , whose support is gratefully acknowledged. This study was supported by research grants from NSERC , the Canadian Space Agency and the University of Winnipeg . Thanks to Thomas McCord and Paul Lucey for highly constructive reviews, and to Christophe Sotin for editorial handling. This research has made use of the NASA Astrophysical Data System. ",

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doi = "10.1016/j.epsl.2014.01.007",

language = "English",

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journal = "Earth and Planetary Science Letters",

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AU - Izawa, Matthew R.M.

AU - Cloutis, Edward A.

AU - Applin, Daniel M.

AU - Craig, Michael A.

AU - Mann, Paul

AU - Cuddy, Matthew

N1 - Funding Information: M.R.M.I. gratefully acknowledges funding from the NSERC CREATE Canadian Astrobiology Training Program and the Mineralogical Association of Canada . The University of Winnipeg's HOSERLab was established with funding from the Canada Foundation for Innovation , the Manitoba Research Innovations Fund and the Canadian Space Agency , whose support is gratefully acknowledged. This study was supported by research grants from NSERC , the Canadian Space Agency and the University of Winnipeg . Thanks to Thomas McCord and Paul Lucey for highly constructive reviews, and to Christophe Sotin for editorial handling. This research has made use of the NASA Astrophysical Data System.

PY - 2014/3/15

Y1 - 2014/3/15

N2 - Reflectance spectroscopy of Apollo lunar soil samples curated in an air- and water-free, sealed environment since recovery and return to Earth has been carried out under water-, oxygen-, CO2- and organic-controlled conditions. Spectra of these pristine samples contain features near 3 μm wavelength similar to those observed from the lunar surface by the Chandrayaan-1 Moon Mineralogy Mapper (M3), Cassini Visual and Infrared Mapping Spectrometer (VIMS), and Deep Impact Extrasolar Planet Observation and Deep Impact Extended Investigation (EPOXI) High-Resolution Instrument (HRI) instruments. Spectral feature characteristics and inferred OH/H2O concentrations are within the range of those observed by spacecraft instruments. These findings confirm that the 3 μm feature from the lunar surface results from the presence of hydration in the form of bound OH and H2O. Implantation of solar wind H+ appears to be the most plausible formation mechanism for most of the observed lunar OH and H2O.

AB - Reflectance spectroscopy of Apollo lunar soil samples curated in an air- and water-free, sealed environment since recovery and return to Earth has been carried out under water-, oxygen-, CO2- and organic-controlled conditions. Spectra of these pristine samples contain features near 3 μm wavelength similar to those observed from the lunar surface by the Chandrayaan-1 Moon Mineralogy Mapper (M3), Cassini Visual and Infrared Mapping Spectrometer (VIMS), and Deep Impact Extrasolar Planet Observation and Deep Impact Extended Investigation (EPOXI) High-Resolution Instrument (HRI) instruments. Spectral feature characteristics and inferred OH/H2O concentrations are within the range of those observed by spacecraft instruments. These findings confirm that the 3 μm feature from the lunar surface results from the presence of hydration in the form of bound OH and H2O. Implantation of solar wind H+ appears to be the most plausible formation mechanism for most of the observed lunar OH and H2O.

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KW - Lunar regolith

KW - Reflectance spectroscopy

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Laboratory spectroscopic detection of hydration in pristine lunar regolith

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