Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
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TY - JOUR
T1 - Mars
T2 - A review and synthesis of general environments and geological settings of magma-H 2O interactions
AU - Head, James W.
AU - Wilson, Lionel
PY - 2002/12/1
Y1 - 2002/12/1
N2 - The advent of a global cryosphere likely occurred very early in the history of Mars, and much of the available water and related volatiles (CO 2, clathrates, etc.) were sequestered within and below the cryosphere. This means that magmatism (plutonism and volcanism) as a geological process throughout the history of Mars cannot be fully understood without accounting for the interaction of magma and water (and related species) in both solid and liquid form. We review and outline the probable configuration of water and ice deposits in the history of Mars, describe environments and modes of magma-H 2O interaction, and provide specific examples from the geological record of Mars. Magma and water-ice interactions have been interpreted to have formed: (1) massive pyroclastic deposits; (2) large-scale ground collapse and chaotic terrain; (3) major outflow channels; (4) mega-lahars dwarfing terrestrial examples; (5) sub-ice-sheet eruptions and edifices; (6) pseudocraters; (7) landslides on volcanic edifice flanks; and (8) hydrothermal sites. The global nature of the cryosphere, its longevity, and the diversity of environments means that Mars is an excellent laboratory for the study of magma-H 2O interactions and the role of related volatile species.
AB - The advent of a global cryosphere likely occurred very early in the history of Mars, and much of the available water and related volatiles (CO 2, clathrates, etc.) were sequestered within and below the cryosphere. This means that magmatism (plutonism and volcanism) as a geological process throughout the history of Mars cannot be fully understood without accounting for the interaction of magma and water (and related species) in both solid and liquid form. We review and outline the probable configuration of water and ice deposits in the history of Mars, describe environments and modes of magma-H 2O interaction, and provide specific examples from the geological record of Mars. Magma and water-ice interactions have been interpreted to have formed: (1) massive pyroclastic deposits; (2) large-scale ground collapse and chaotic terrain; (3) major outflow channels; (4) mega-lahars dwarfing terrestrial examples; (5) sub-ice-sheet eruptions and edifices; (6) pseudocraters; (7) landslides on volcanic edifice flanks; and (8) hydrothermal sites. The global nature of the cryosphere, its longevity, and the diversity of environments means that Mars is an excellent laboratory for the study of magma-H 2O interactions and the role of related volatile species.
U2 - 10.1144/GSL.SP.2002.202.01.03
DO - 10.1144/GSL.SP.2002.202.01.03
M3 - Journal article
AN - SCOPUS:0037004949
VL - 202
SP - 27
EP - 57
JO - Geological Society Special Publication
JF - Geological Society Special Publication
SN - 0305-8719
ER -