Solar System Research

, Volume 48, Issue 6, pp 391–402

Geological context of potential landing site of the Luna-Glob mission

  • M. A. Ivanov
  • A. M. Abdrakhimov
  • A. T. Basilevsky
  • J. L. Dixon
  • J. W. Head
  • L. Chick
  • J. Vitten
  • M. T. Zuber
  • D. E. Simt
  • E. Mazarico
  • C. D. Neish
  • D. B. J. Bassey
Article

DOI: 10.1134/S0038094614060021

Cite this article as:
Ivanov, M.A., Abdrakhimov, A.M., Basilevsky, A.T. et al. Sol Syst Res (2014) 48: 391. doi:10.1134/S0038094614060021

Abstract

The region planned for performing the Luna-Glob mission is located in the southern part of the swell surrounding the largest South Pole-Aitken (SPA) basin. The photogeological analysis of the surface topography of this region using the LRO-WAC (resolution of 100 Mpxl) photomaps made it possible to define the following groups of morphological units (area types): (1) related to the formation of relatively fresh impact craters; (2) associated with larger (>100 km across) degraded craters including (2a) external and (2b) inner facies; and (3) occupying intercrater spaces. The comparison of the geological map with the map illustrating the distribution of the epithermal neutron flow (Mitrofanov et al., 2012) shows no correlation between them. Consequently, one should not expect development of rock complexes, which would be characterized by elevated concentrations of water in the region chosen for the Luna-Glob mission and, thus, considered among the first-priority targets. The comparison of the neutron flow distribution with the map of circular polarization of the Mini-RF radar beam also shows no correlation. This means that high values of circular polarization reflect elevated concentrations of rock fragments rather than water accumulations. Even though ice fragments are present, their sizes should only slightly be less as compared with the radar wavelength (12.6 cm). The region planned for investigations in the scope of the Luna-Glob mission corresponds to the swell of the largest (and, likely, oldest) preserved basin and offers a potential opportunity to analyze ancient material of this planet and introduce important constraints into the spectrum of models proposed for explaining the Moon’s origin.

Copyright information

© Pleiades Publishing, Inc. 2014

Authors and Affiliations

  • M. A. Ivanov
    • 1
    • 2
    • 3
  • A. M. Abdrakhimov
    • 1
    • 2
  • A. T. Basilevsky
    • 1
    • 2
    • 3
  • J. L. Dixon
    • 2
  • J. W. Head
    • 2
  • L. Chick
    • 2
  • J. Vitten
    • 2
  • M. T. Zuber
    • 4
  • D. E. Simt
    • 5
  • E. Mazarico
    • 5
  • C. D. Neish
    • 6
  • D. B. J. Bassey
    • 7
  1. 1.Vernadsky Institute of Geochemistry and Analytical ChemistryRussian Academy of SciencesMoscowRussia
  2. 2.Brown UniversityProvidenceUSA
  3. 3.Moscow State University of Geodesy and CartographyMoscowRussia
  4. 4.Massachusetts Institute of TechnologyBostonUSA
  5. 5.Goddard CenterGreenbeltUSA
  6. 6.Florida Institute of TechnologyMelbourneUSA
  7. 7.Laboratory of Applied PhysicsJohn Hopkins UniversityWashingtonUSA

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