Chronology and Evolution of Mars: Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland
Gespeichert in:
| 1. Verfasser: | |
|---|---|
| Format: | Elektronisch E-Book |
| Sprache: | English |
| Veröffentlicht: |
Dordrecht
Springer Netherlands
2001
|
| Schriftenreihe: | Space Sciences Series of ISSI
12 |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Beschreibung: | 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 |
| Beschreibung: | 1 Online-Ressource (X, 500 p) |
| ISBN: | 9789401710350 9789048157259 |
| ISSN: | 1385-7525 |
| DOI: | 10.1007/978-94-017-1035-0 |
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| 246 | 1 | 3 | |a Proceedings from an ISSI workshop, 10-14 April 2000, Bern, Switzerland |
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| 500 | |a 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 | ||
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Datensatz im Suchindex
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| author | Kallenbach, Reinald |
| author_facet | Kallenbach, Reinald |
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| building | Verbundindex |
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| dewey-full | 523.01 |
| dewey-hundreds | 500 - Natural sciences and mathematics |
| dewey-ones | 523 - Specific celestial bodies and phenomena |
| dewey-raw | 523.01 |
| dewey-search | 523.01 |
| dewey-sort | 3523.01 |
| dewey-tens | 520 - Astronomy and allied sciences |
| discipline | Physik |
| doi_str_mv | 10.1007/978-94-017-1035-0 |
| format | Electronic eBook |
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| geographic | Mars Planet (DE-588)4037687-4 gnd |
| geographic_facet | Mars Planet |
| id | DE-604.BV042416267 |
| illustrated | Not Illustrated |
| indexdate | 2024-07-10T01:20:59Z |
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| isbn | 9789401710350 9789048157259 |
| issn | 1385-7525 |
| language | English |
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| spelling | Kallenbach, Reinald Verfasser aut Chronology and Evolution of Mars Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland edited by Reinald Kallenbach, Johannes Geiss, William K. Hartmann Proceedings from an ISSI workshop, 10-14 April 2000, Bern, Switzerland Dordrecht Springer Netherlands 2001 1 Online-Ressource (X, 500 p) txt rdacontent c rdamedia cr rdacarrier Space Sciences Series of ISSI 12 1385-7525 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 Physics Geochemistry Planetology Astrophysics and Astroparticles Geologie (DE-588)4020227-6 gnd rswk-swf Mars Planet (DE-588)4037687-4 gnd rswk-swf 1\p (DE-588)1071861417 Konferenzschrift 2000 Bern gnd-content Mars Planet (DE-588)4037687-4 g Geologie (DE-588)4020227-6 s 2\p DE-604 Geiss, Johannes Sonstige oth Hartmann, William K. Sonstige oth https://doi.org/10.1007/978-94-017-1035-0 Verlag Volltext 1\p cgwrk 20201028 DE-101 https://d-nb.info/provenance/plan#cgwrk 2\p cgwrk 20201028 DE-101 https://d-nb.info/provenance/plan#cgwrk |
| spellingShingle | Kallenbach, Reinald Chronology and Evolution of Mars Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland Physics Geochemistry Planetology Astrophysics and Astroparticles Geologie (DE-588)4020227-6 gnd |
| subject_GND | (DE-588)4020227-6 (DE-588)4037687-4 (DE-588)1071861417 |
| title | Chronology and Evolution of Mars Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland |
| title_alt | Proceedings from an ISSI workshop, 10-14 April 2000, Bern, Switzerland |
| title_auth | Chronology and Evolution of Mars Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland |
| title_exact_search | Chronology and Evolution of Mars Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland |
| title_full | Chronology and Evolution of Mars Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland edited by Reinald Kallenbach, Johannes Geiss, William K. Hartmann |
| title_fullStr | Chronology and Evolution of Mars Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland edited by Reinald Kallenbach, Johannes Geiss, William K. Hartmann |
| title_full_unstemmed | Chronology and Evolution of Mars Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland edited by Reinald Kallenbach, Johannes Geiss, William K. Hartmann |
| title_short | Chronology and Evolution of Mars |
| title_sort | chronology and evolution of mars proceedings of an issi workshop 10 14 april 2000 bern switzerland |
| title_sub | Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland |
| topic | Physics Geochemistry Planetology Astrophysics and Astroparticles Geologie (DE-588)4020227-6 gnd |
| topic_facet | Physics Geochemistry Planetology Astrophysics and Astroparticles Geologie Mars Planet Konferenzschrift 2000 Bern |
| url | https://doi.org/10.1007/978-94-017-1035-0 |
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