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Chronology and Evolution of Mars

Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland

  • Reinald Kallenbach
  • Johannes Geiss
  • William K. Hartmann

Part of the Space Sciences Series of ISSI book series (SSSI, volume 12)

Table of contents

  1. Front Matter
    Pages i-ix
  2. Introduction: A New Chapter in Mars Research

    1. Reinald Kallenbach, Johannes Geiss, William K. Hartmann
      Pages 3-6
  3. Chronology of Mars and of the Inner Solar System

    1. Front Matter
      Pages 7-7
    2. Boris A. Ivanov
      Pages 87-104
    3. L. E. Nyquist, D. D. Bogard, C.-Y. Shih, A. Greshake, D. Stöffler, O. Eugster
      Pages 105-164
    4. William K. Hartmann, Gerhard Neukum
      Pages 165-194
  4. Evolution of the Interior and Surface of Mars

    1. Front Matter
      Pages 195-195
    2. A. N. Halliday, H. Wänke, J.-L. Birck, R. N. Clayton
      Pages 197-230
    3. Tilman Spohn, Mario H. Acuña, Doris Breuer, Matthew Golombek, Ronald Greeley, Alexander Halliday et al.
      Pages 231-262
    4. J. W. Head, R. Greeley, M. P. Golombek, W. K. Hartmann, E. Hauber, R. Jaumann et al.
      Pages 263-292
    5. Jean-Pierre Bibring, Stéphane Erard
      Pages 293-316
    6. H. Wänke, J. Brückner, G. Dreibus, R. Rieder, I. Ryabchikov
      Pages 317-330
  5. History and Fate of the Martian Atmosphere and Hydrosphere

    1. Front Matter
      Pages 331-331
    2. Philippe Masson, Michael H. Carr, François Costard, Ronald Greeley, Ernst Hauber, Ralf Jaumann
      Pages 333-364
    3. J. C. Bridges, D. C. Catling, J. M. Saxton, T. D. Swindle, I. C. Lyon, M. M. Grady
      Pages 365-392
    4. Ronald Greeley, Ruslan O. Kuzmin, Robert M. Haberle
      Pages 393-404
    5. D. D. Bogard, R. N. Clayton, K. Marti, T. Owen, G. Turner
      Pages 425-458
  6. Epilogue

    1. Front Matter
      Pages 459-459
    2. W. K. Hartmann, R. Kallenbach, J. Geiss, G. Turner
      Pages 461-470
  7. Back Matter
    Pages 471-499

About these proceedings

Introduction

Mars is about one-eighth the mass of the Earth and it may provide an analogue of what the Earth was like when it was at such an early stage of accretion. The fur­ ther growth of the Earth was sustained by major collisions with planetesimals and planets such as that which resulted in the formation ofthe Earth's moon (Hartmann and Davis, 1975; Cameron and Ward, 1976; Wetherill, 1986; Cameron and Benz, 1991). This late accretionary history, which lasted more than 50 Myr in the case of the Earth (Halliday, 2000a, b), appears to have been shorter and less catastrophic in the case of Mars (Harper et ai. , 1995; Lee and Halliday, 1997). In this article we review the basic differences between the bulk composition of Mars and the Earth and the manner in which this plays into our understanding of the timing and mechanisms of accretion and core formation. We highlight some of the evidence for early cessation of major collisional growth on Mars. Finally, we reevaluate the isotopic evidence that Mars differentiated quickly. Fundamental differences between the composition of Mars and that of other terrestrial planets are apparent from the planet's slightly lower density and from the compositions of Martian meteorites. The low density is partially explicable if there is a greater proportion of more volatile elements.

Keywords

Accretion Solar System atmosphere solar space science

Editors and affiliations

  • Reinald Kallenbach
    • 1
  • Johannes Geiss
    • 1
  • William K. Hartmann
    • 2
  1. 1.International Space Science InstituteBernSwitzerland
  2. 2.Planetary Science InstituteTucsonUSA

Bibliographic information

  • DOI https://doi.org/10.1007/978-94-017-1035-0
  • Copyright Information Springer Science+Business Media Dordrecht 2001
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-90-481-5725-9
  • Online ISBN 978-94-017-1035-0
  • Series Print ISSN 1385-7525
  • Buy this book on publisher's site
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