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The Surface Composition of Ceres

  • Chapter
The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres

Abstract

Our understanding of the composition of Ceres is driven by remote sensing of its surface. We review spectral observations of Ceres over wavelengths from the ultraviolet to the radio, as well as non-spectral data such as thermal inertia, photometric properties, radar experiments, and surface variability. We also discuss the closest likely meteorite analogs to Ceres and consider the likelihood that material from Ceres could be delivered to Earth.

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Author information

Authors and Affiliations

  1. Applied Physics Laboratory, Johns Hopkins University, Laurel, MD, USA

    Andrew S. Rivkin

  2. University of Maryland, College Park, MD, USA

    Jian-Yang Li & Lucy A. McFadden

  3. University of Notre Dame, Notre Dame, IN, USA

    Ralph E. Milliken

  4. NASA Goddard Space Flight Center, Greenbelt, MD, USA

    Lucy F. Lim

  5. Agnes Scott College, Atlanta, GA, USA

    Amy J. Lovell

  6. University of California Los Angeles, Los Angeles, CA, USA

    Britney E. Schmidt

  7. NASA Marshall Space Flight Center, Huntsville, AL, USA

    Barbara A. Cohen

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Corresponding author

Correspondence to Andrew S. Rivkin .

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Editors and Affiliations

  1. Department of Earth and Space Sciences, Institute Geophysics & Planetary Physics, University of California Los Angeles, Los Angeles, CA, USA

    Christopher Russell

  2. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA

    Carol Raymond

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Rivkin, A.S. et al. (2010). The Surface Composition of Ceres. In: Russell, C., Raymond, C. (eds) The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres. Springer, New York, NY. https://doi.org/10.1007/978-1-4614-4903-4_7

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