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Earth-Moon Relationships

Proceedings of the Conference held in Padova, Italy at the Accademia Galileiana di Scienze Lettere ed Arti, November 8–10, 2000

  • Cesare Barbieri
  • Francesca Rampazzi

Table of contents

  1. Front Matter
    Pages i-x
  2. Oral Contributions

    1. Cesare Barbieri
      Pages 1-3
    2. Claudio Bellinati
      Pages 45-50
    3. C. R. Benn
      Pages 61-66
    4. Dario Camuffo
      Pages 99-113
    5. Mark Deantonio
      Pages 129-131
    6. B. H. Foing, M. Duke, E. Galimov, H. Mizutani, C. Pieters, G. Racca et al.
      Pages 133-142
    7. M. Jourdain De Muizon, R. J. Laureijs, H. J. Habing, K. Leech, M. F. Kessler, L. Metcalfe et al.
      Pages 201-207
    8. Oddone Longo
      Pages 237-243
    9. Michael Mendillo
      Pages 271-277
    10. Elfed Morgan
      Pages 279-290
    11. Roberta J. M. Olson, Jay M. Pasachoff
      Pages 303-341
    12. Tobias Owen, Hasso Niemann, Paul Mahaffy
      Pages 343-350
    13. Luigi Peruzzo, Denis Bastieri
      Pages 351-362
    14. Giuseppe D. Racca, Bernard H. Foing, Marcello Coradini
      Pages 379-390
    15. Wolfgang Schad
      Pages 405-409
    16. David R. Scott
      Pages 411-418
    17. Guido Tagliaferri, Pasquale Tucci
      Pages 427-441
    18. G. B. Valsecchi
      Pages 443-443
  3. Posters

    1. Cesare Barbieri, Chris R. Benn, Gabriele Cremonese, Stefano Verani, Alberto Zin
      Pages 479-486
    2. Cesare Barbieri, Sonia Fornasier, Monica Lazzarin, Simone Marchi, Francesca Rampazzi, Stefano Verani et al.
      Pages 487-495
    3. C. R. Benn
      Pages 497-498
    4. Francesco Bertola
      Pages 505-513
    5. Massimo Capaccioli, Emilia Olostro Cirella, Enrica Stendardo, Nicla Virgilio
      Pages 515-515
    6. Pierantonio Cinzano, Fabio Falchi, Christopher D. Elvidge
      Pages 517-522
    7. B. H. Foing, D. J. Heather, M. Almeida, SMART-1 Science Technology Working Team
      Pages 523-531

About these proceedings

Introduction

Sediments and sedimentary processes on the Moon and Earth are very different. In the absence of water, an atmosphere, the magnetosphere, and much less oxygen in its rocks, the Moon has neither clay minerals nor carbonates, and no Fe3+. Mechanical weathering by impacts is the principal process of sediment generation on the Moon; on Earth, chemical weathering predominates. Whereas processes of sediment transport are principally ballistic on the Moon, movement by air, water and ice prevail on the Earth. The radical differences between Earth and Moon sediments make them useful end-members between which all sediments of all terrestrial planetary bodies are expected to lie. The purpose of this paper is (l) to compare and contrast major characteristics of the origin, transportation, deposition, and preservation of sediments, especially dust, in the Earth and the Moon, and (2) to suggest how sediments of other rocky planetary bodies, especially Mars, may fit in-between the sediments of the Earth and the Moon.

Keywords

Map Planet Solar System astronomy biology solar theory

Editors and affiliations

  • Cesare Barbieri
    • 1
  • Francesca Rampazzi
    • 2
  1. 1.Department of AstronomyUniversity of PadovaPadovaItaly
  2. 2.C.I.S.A.S.University of PadovaPadovaItaly

Bibliographic information

  • DOI https://doi.org/10.1007/978-94-010-0800-6
  • Copyright Information Springer Science+Business Media B.V. 2001
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-94-010-3855-3
  • Online ISBN 978-94-010-0800-6
  • Buy this book on publisher's site
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