Advances in aqueous minerals detection on Martian surface

  • role: First author第一作者
  • Affiliation:

    State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, Beijing 100101, China

  • Email:gousheng@radi.ac.cn
  • Introduction:芶盛(1985— ),男,助理研究员,研究方向为遥感地质与深空探测。E-mail:gousheng@radi.ac.cn
GOU Sheng,  
  • Affiliation:

    State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, Beijing 100101, China

YUE Zongyu,  
  • role: Corresponding author通信作者
  • Affiliation:

    State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, Beijing 100101, China

  • Email:dikc@radi.ac.cn
  • Introduction:邸凯昌(1967— ),男,研究员,研究方向为行星遥感制图与导航定位。E-mail:dikc@radi.ac.cn
DI Kaichang*,  
  • Affiliation:

    State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, Beijing 100101, China

ZHANG Xia

resumen

Aqueous minerals are either minerals that form in water or formations that are related to water. The type of aqueous mineral depends on temperature, salinity, PH, and composition of the parent rock at their forming time, which provides important clues to understanding the past aqueous environments of Mars, delineating advantageous regions for life activities, and even searching for possible existing Martian life. Therefore, studies on aqueous mineral identification and spatial distribution pattern are of considerable scientific significances. This paper provides a comprehensive overview of the advances of aqueous minerals detection on Martian surface since the 1990s. First, the major specifications of two data sources for mineral detection are introduced, including orbital spectrometers (TES, THEMIS, OMEGA, and CRISM) and in-situ landers/rovers (MPF/Sojourner, Spirit, Opportunity, Phoenix, and Curiosity). The spectrometers utilize either emission features in thermal infrared (TIR) or reflectance absorption characteristics in visible/near-infrared (VNIR) to identify and discriminate mineral types. Landers and rovers equipped with scientific instruments carry out the in-situ measurement to provide detailed component identification, abundance detection, and other analyses on the Martian surface soil, minerals, and rocks. Second, the spectral features, specific types, and distribution patterns of aqueous minerals detected on Martian surface are illustrated in detail as bound water, adsorbed water, and structural OH in aqueous minerals can be remotely detected via their unique spectral characteristics. Although aqueous minerals are widespread on Mars, they are concentrated in the Noachian southern highlands. At present, the aqueous minerals detected and verified on Martian surface from orbital spectrometers and landers/rovers can be classified as hydrous silicate minerals, sulfates, carbonates, chlorides, and perchlorates. Third, the major aqueous mineral quantitative retrieval methods, including absorption band depth conversion and spectral unmixing algorithms, are introduced. Compared with the linear unmixing model, the nonlinear spectral unmixing model can characterize mineral composition and retrieval mineral abundance with higher precision; therefore, it has been extensively used for the quantitative retrieval of aqueous mineral on Martian surface. The most commonly used nonlinear spectral unmixing models are the Hapke and Shkuratov models. The retrieval works provide fine quantitative data for inferring the formation and evolution history of aqueous mineral on Martian surface. However, numerous limitations exist, which are still important and difficult issues in aqueous mineral detection and retrieval via remote sensing. Furthermore, the retrieval advances at global and local scales, as well as their geological implications for Mars, are summarized. The detection of aqueous minerals confirms the existence of past water solution environment on Martian surface, and the phenomenon of diverse aqueous mineral categories that formed in various geomorphologies and geological contexts gradually changes over time reveals the evolution diversity of the chemical properties of water solution. Considering these two conditions, the paper finally proposes an analog study between Earth and Mars that should be carried out from the viewpoint of comparative planetology on the formation environment and process of aqueous minerals, which has important reference significance for the Mars exploration mission of China that is planned to be launched in 2020.

palabra clave

Martian surface;aqueous mineral;remote sensing detection;in-situ detection;quantitative retrieval;comparative planetology

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