Overview
- Editors:
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Reinald Kallenbach
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International Space Science Institute, Bern, Switzerland
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Johannes Geiss
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International Space Science Institute, Bern, Switzerland
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William K. Hartmann
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Planetary Science Institute, Tucson, USA
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Table of contents (18 papers)
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Introduction: A New Chapter in Mars Research
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- Reinald Kallenbach, Johannes Geiss, William K. Hartmann
Pages 3-6
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Chronology of Mars and of the Inner Solar System
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- Dieter Stöffler, G. Ryder
Pages 9-54
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- G. Neukum, B. A. Ivanov, W. K. Hartmann
Pages 55-86
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- L. E. Nyquist, D. D. Bogard, C.-Y. Shih, A. Greshake, D. Stöffler, O. Eugster
Pages 105-164
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- William K. Hartmann, Gerhard Neukum
Pages 165-194
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Evolution of the Interior and Surface of Mars
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Front Matter
Pages 195-195
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- A. N. Halliday, H. Wänke, J.-L. Birck, R. N. Clayton
Pages 197-230
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- Tilman Spohn, Mario H. Acuña, Doris Breuer, Matthew Golombek, Ronald Greeley, Alexander Halliday et al.
Pages 231-262
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- J. W. Head, R. Greeley, M. P. Golombek, W. K. Hartmann, E. Hauber, R. Jaumann et al.
Pages 263-292
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- Jean-Pierre Bibring, Stéphane Erard
Pages 293-316
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- H. Wänke, J. Brückner, G. Dreibus, R. Rieder, I. Ryabchikov
Pages 317-330
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History and Fate of the Martian Atmosphere and Hydrosphere
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Front Matter
Pages 331-331
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- Philippe Masson, Michael H. Carr, François Costard, Ronald Greeley, Ernst Hauber, Ralf Jaumann
Pages 333-364
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- J. C. Bridges, D. C. Catling, J. M. Saxton, T. D. Swindle, I. C. Lyon, M. M. Grady
Pages 365-392
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- Ronald Greeley, Ruslan O. Kuzmin, Robert M. Haberle
Pages 393-404
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About this book
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.