Impact-generated hydrothermal systems on Earth and Mars
It has long been suggested that hydrothermal systems might have provided habitats for the origin and evolution of early life on Earth, and possibly other planets such as Mars. In this contribution we show that most impact events that result in the formation of complex impact craters (i.e., >2-4 a...
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Language: | English |
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2013
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Online Access: | https://espace.library.uq.edu.au/view/UQ:315075 |
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ftunivqespace:oai:espace.library.uq.edu.au:UQ:315075 2023-05-15T16:00:47+02:00 Impact-generated hydrothermal systems on Earth and Mars Osinski, Gordon R. Tornabene, Livio L. Banerjee, Neil R. Cockell, Charles S. Flemming, Roberta Izawa, Matthew R. M. McCutcheon, Jenine Parnell, John Preston, Louisa J. Pickersgill, Annemarie E. Pontefract, Alexandra Sapers, Haley M. Southam, Gordon 2013-06-01 https://espace.library.uq.edu.au/view/UQ:315075 eng eng Academic Press doi:10.1016/j.icarus.2012.08.030 issn:0019-1035 issn:1090-2643 orcid:0000-0002-8941-1249 Not set Impact processes Cratering Mars Astrobiology Devon Island 1912 Space and Planetary Science 3103 Astronomy and Astrophysics Journal Article 2013 ftunivqespace https://doi.org/10.1016/j.icarus.2012.08.030 2020-12-15T00:40:48Z It has long been suggested that hydrothermal systems might have provided habitats for the origin and evolution of early life on Earth, and possibly other planets such as Mars. In this contribution we show that most impact events that result in the formation of complex impact craters (i.e., >2-4 and >5-10. km diameter on Earth and Mars, respectively) are potentially capable of generating a hydrothermal system. Consideration of the impact cratering record on Earth suggests that the presence of an impact crater lake is critical for determining the longevity and size of the hydrothermal system. We show that there are six main locations within and around impact craters on Earth where impact-generated hydrothermal deposits can form: (1) crater-fill impact melt rocks and melt-bearing breccias; (2) interior of central uplifts; (3) outer margin of central uplifts; (4) impact ejecta deposits; (5) crater rim region; and (6) post-impact crater lake sediments. We suggest that these six locations are applicable to Mars as well. Evidence for impact-generated hydrothermal alteration ranges from discrete vugs and veins to pervasive alteration depending on the setting and nature of the system. A variety of hydrothermal minerals have been documented in terrestrial impact structures and these can be grouped into three broad categories: (1) hydrothermally-altered target-rock assemblages; (2) primary hydrothermal minerals precipitated from solutions; and (3) secondary assemblages formed by the alteration of primary hydrothermal minerals. Target lithology and the origin of the hydrothermal fluids strongly influences the hydrothermal mineral assemblages formed in these post-impact hydrothermal systems. There is a growing body of evidence for impact-generated hydrothermal activity on Mars; although further detailed studies using high-resolution imagery and multispectral information are required. Such studies have only been done in detail for a handful of martian craters. The best example so far is from Toro Crater (Marzo, G.A., Davila, A.F., Tornabene, L.L., Dohm, J.M., Fairèn, A.G., Gross, C., Kneissl, T., Bishop, J.L., Roush, T.L., Mckay, C.P. [2010]. Icarus 208, 667-683). We also present new evidence for impact-generated hydrothermal deposits within an unnamed ∼32-km diameter crater ∼350. km away from Toro and within the larger Holden Crater. Synthesizing observations of impact craters on Earth and Mars, we suggest that if there was life on Mars early in its history, then hydrothermal deposits associated with impact craters may provide the best, and most numerous, opportunities for finding preserved evidence for life on Mars. Moreover, hydrothermally altered and precipitated rocks can provide nutrients and habitats for life long after hydrothermal activity has ceased. Article in Journal/Newspaper Devon Island The University of Queensland: UQ eSpace Crater Lake ENVELOPE(-60.667,-60.667,-62.983,-62.983) Devon Island ENVELOPE(-88.000,-88.000,75.252,75.252) Target Rock ENVELOPE(-92.851,-92.851,63.876,63.876) Icarus 224 2 347 363 |
institution |
Open Polar |
collection |
The University of Queensland: UQ eSpace |
op_collection_id |
ftunivqespace |
language |
English |
topic |
Impact processes Cratering Mars Astrobiology Devon Island 1912 Space and Planetary Science 3103 Astronomy and Astrophysics |
spellingShingle |
Impact processes Cratering Mars Astrobiology Devon Island 1912 Space and Planetary Science 3103 Astronomy and Astrophysics Osinski, Gordon R. Tornabene, Livio L. Banerjee, Neil R. Cockell, Charles S. Flemming, Roberta Izawa, Matthew R. M. McCutcheon, Jenine Parnell, John Preston, Louisa J. Pickersgill, Annemarie E. Pontefract, Alexandra Sapers, Haley M. Southam, Gordon Impact-generated hydrothermal systems on Earth and Mars |
topic_facet |
Impact processes Cratering Mars Astrobiology Devon Island 1912 Space and Planetary Science 3103 Astronomy and Astrophysics |
description |
It has long been suggested that hydrothermal systems might have provided habitats for the origin and evolution of early life on Earth, and possibly other planets such as Mars. In this contribution we show that most impact events that result in the formation of complex impact craters (i.e., >2-4 and >5-10. km diameter on Earth and Mars, respectively) are potentially capable of generating a hydrothermal system. Consideration of the impact cratering record on Earth suggests that the presence of an impact crater lake is critical for determining the longevity and size of the hydrothermal system. We show that there are six main locations within and around impact craters on Earth where impact-generated hydrothermal deposits can form: (1) crater-fill impact melt rocks and melt-bearing breccias; (2) interior of central uplifts; (3) outer margin of central uplifts; (4) impact ejecta deposits; (5) crater rim region; and (6) post-impact crater lake sediments. We suggest that these six locations are applicable to Mars as well. Evidence for impact-generated hydrothermal alteration ranges from discrete vugs and veins to pervasive alteration depending on the setting and nature of the system. A variety of hydrothermal minerals have been documented in terrestrial impact structures and these can be grouped into three broad categories: (1) hydrothermally-altered target-rock assemblages; (2) primary hydrothermal minerals precipitated from solutions; and (3) secondary assemblages formed by the alteration of primary hydrothermal minerals. Target lithology and the origin of the hydrothermal fluids strongly influences the hydrothermal mineral assemblages formed in these post-impact hydrothermal systems. There is a growing body of evidence for impact-generated hydrothermal activity on Mars; although further detailed studies using high-resolution imagery and multispectral information are required. Such studies have only been done in detail for a handful of martian craters. The best example so far is from Toro Crater (Marzo, G.A., Davila, A.F., Tornabene, L.L., Dohm, J.M., Fairèn, A.G., Gross, C., Kneissl, T., Bishop, J.L., Roush, T.L., Mckay, C.P. [2010]. Icarus 208, 667-683). We also present new evidence for impact-generated hydrothermal deposits within an unnamed ∼32-km diameter crater ∼350. km away from Toro and within the larger Holden Crater. Synthesizing observations of impact craters on Earth and Mars, we suggest that if there was life on Mars early in its history, then hydrothermal deposits associated with impact craters may provide the best, and most numerous, opportunities for finding preserved evidence for life on Mars. Moreover, hydrothermally altered and precipitated rocks can provide nutrients and habitats for life long after hydrothermal activity has ceased. |
format |
Article in Journal/Newspaper |
author |
Osinski, Gordon R. Tornabene, Livio L. Banerjee, Neil R. Cockell, Charles S. Flemming, Roberta Izawa, Matthew R. M. McCutcheon, Jenine Parnell, John Preston, Louisa J. Pickersgill, Annemarie E. Pontefract, Alexandra Sapers, Haley M. Southam, Gordon |
author_facet |
Osinski, Gordon R. Tornabene, Livio L. Banerjee, Neil R. Cockell, Charles S. Flemming, Roberta Izawa, Matthew R. M. McCutcheon, Jenine Parnell, John Preston, Louisa J. Pickersgill, Annemarie E. Pontefract, Alexandra Sapers, Haley M. Southam, Gordon |
author_sort |
Osinski, Gordon R. |
title |
Impact-generated hydrothermal systems on Earth and Mars |
title_short |
Impact-generated hydrothermal systems on Earth and Mars |
title_full |
Impact-generated hydrothermal systems on Earth and Mars |
title_fullStr |
Impact-generated hydrothermal systems on Earth and Mars |
title_full_unstemmed |
Impact-generated hydrothermal systems on Earth and Mars |
title_sort |
impact-generated hydrothermal systems on earth and mars |
publisher |
Academic Press |
publishDate |
2013 |
url |
https://espace.library.uq.edu.au/view/UQ:315075 |
long_lat |
ENVELOPE(-60.667,-60.667,-62.983,-62.983) ENVELOPE(-88.000,-88.000,75.252,75.252) ENVELOPE(-92.851,-92.851,63.876,63.876) |
geographic |
Crater Lake Devon Island Target Rock |
geographic_facet |
Crater Lake Devon Island Target Rock |
genre |
Devon Island |
genre_facet |
Devon Island |
op_relation |
doi:10.1016/j.icarus.2012.08.030 issn:0019-1035 issn:1090-2643 orcid:0000-0002-8941-1249 Not set |
op_doi |
https://doi.org/10.1016/j.icarus.2012.08.030 |
container_title |
Icarus |
container_volume |
224 |
container_issue |
2 |
container_start_page |
347 |
op_container_end_page |
363 |
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1766396806517751808 |