Mars Surface Diversity as Revealed by the OMEGA/Mars Express Observations-Reference-Cited by-同舟云学术

Mars Surface Diversity as Revealed by the OMEGA/Mars Express Observations

Published:2005-03-11 Issue:5715 Volume:307 Page:1576-1581
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Bibring Jean-Pierre¹²³⁴⁵,Langevin Yves¹²³⁴⁵,Gendrin Aline¹²³⁴⁵,Gondet Brigitte¹²³⁴⁵,Poulet François¹²³⁴⁵,Berthé Michel¹²³⁴⁵,Soufflot Alain¹²³⁴⁵,Arvidson Ray¹²³⁴⁵,Mangold Nicolas¹²³⁴⁵,Mustard John¹²³⁴⁵,Drossart P.¹²³⁴⁵,

Affiliation:

1. Institut d'Astrophysique Spatiale (IAS), Bâtiment 121, 91405 Orsay Campus, France.

2. Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA.

3. Interactions et Dynamique des Environnements de Surface (IDES), Bâtiment 509, 91405 Orsay Campus, France.

4. Geological Sciences, Brown University, Providence, RI 02912, USA.

5. Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, 92195 Meudon, France.

Abstract

The Observatoire pour la Minéralogie, l'Eau, les Glaces, et l'Activité (OMEGA) investigation, on board the European Space Agency Mars Express mission, is mapping the surface composition of Mars at a 0.3- to 5-kilometer resolution by means of visible–near-infrared hyperspectral reflectance imagery. The data acquired during the first 9 months of the mission already reveal a diverse and complex surface mineralogy, offering key insights into the evolution of Mars. OMEGA has identified and mapped mafic iron-bearing silicates of both the northern and southern crust, localized concentrations of hydrated phyllosilicates and sulfates but no carbonates, and ices and frosts with a water-ice composition of the north polar perennial cap, as for the south cap, covered by a thin carbon dioxide–ice veneer.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference33 articles.

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3. Olivine and Pyroxene Diversity in the Crust of Mars

4. The Martian chronology is described in three epochs on the basis of the density of impact craters identified on optical images. The first epoch named Noachian corresponds to the early heavy bombardment which ended ∼3.8 billion years ago (Noachis is a region located within the highly cratered terrains which still cover ∼40% of the Mars surface primarily in the south). The second period or Hesperian (named after Hesperia Planitia as a typical area of this age) lasted until ∼2 billion years. It is followed by the most recent Amazonian period (Amazonia Planitia belongs to the least cratered volcanic plain).

5. A Global View of Martian Surface Compositions from MGS-TES

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