Shape, rheology and emplacement times of small martian shield volcanoes

Baratoux, D.; Pinet, P.; Toplis, Michael J.; Mangold, N.; Greeley, R.; Baptista, A. R.

doi:10.1016/j.jvolgeores.2009.05.003

Cited by 35 publications

(15 citation statements)

References 34 publications

(53 reference statements)

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“…Ultimately, schwertmannite may convert to hydrous ferric oxides such as ferrihydrite and goethite, which Weathering experiments of basaltic rocks (Nesbith and Young 1984;Nesbith and Wilson 1992;Gislasson and Arnolsson 1993;Tosca et al 2004;Golden et al 2005;Hausrath et al 2013) and olivine (King et al 2011) suggest that the bulk composition of the starting material, low water/rock ratios and incongruent rock or glass dissolution may lead to the formation of magnesium sulfates. Mars is largely a basaltic planet (Baratoux et al 2009;Carr and Head 2010;Grott et al 2013) whereas silicic and intermediate rocks predominate on the continents of the earth. Some of these major differences in surface rocks between the two planets are reflected in their secondary minerals.…”

Section: Comparison Between Mineralogical Features Of Copahue-caviahumentioning

confidence: 99%

Acid Rivers and Lakes at Caviahue-Copahue Volcano as Potential Terrestrial Analogues for Aqueous Paleo-Environments on Mars

Aguilar

Varekamp

Bergen

et al. 2015

Active Volcanoes of the World

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Mars carries primary rock with patchy occurrences of sulfates and sheet silicates. Both Mg-and Fe-sulfates have been documented, the former being rather uncommon on Earth. To what extent can a natural acidic river system on Earth be a terrestrial analog for early Mars environments? Copahue volcano (Argentina) has an active acid hydrothermal system that has precipitated a suite of minerals in its hydrothermal reservoir (silica, anhydrite, alunite, jarosite). Leakage from this subterranean system through hot springs and into the crater lake have formed a strongly acidified watershed (Río Agrio), which precipitates a host of minerals during cooling and dilution downstream. A suite of more than 100 minerals has been found and conditions for precipitation of the main phases are simulated with speciation/saturation routines. The lower part of the watershed (Lake Caviahue and the Lower Río Agrio) have abundant deposits of ferricrete since 2003: hydrous ferric oxides and schwertmannite occur, their precipitation being mediated by Fe-oxidizing bacteria and photochemical processes. Further downstream, at greater degrees of dilution, hydrous aluminum oxides and sulfates form and create 'alcretes' lining the river bed. The watershed carries among others jarosite, hematite, anhydrite, gypsum and silica minerals and the origin of all these minerals

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Section: Comparison Between Mineralogical Features Of Copahue-caviahumentioning

confidence: 99%

Acid Rivers and Lakes at Caviahue-Copahue Volcano as Potential Terrestrial Analogues for Aqueous Paleo-Environments on Mars

Aguilar

Varekamp

Bergen

et al. 2015

Active Volcanoes of the World

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“…25). This period is marked by activity of giant shield volcanoes (Olympus Mons, Elysium Mons, Arsia Mons) that are up to 500 km in diameter and 25 km in height, and formation of numerous smaller shield volcanoes (Plescia 1990;Hauber et al 2009Hauber et al , 2011Vaucher et al 2009;Baratoux et al 2009;Platz and Michael 2011) and local explosive activity (e.g., Hauber et al 2005). Shield volcanoes (typically 5-10 • in average slope) have been fed by continuous magmatism over millions of years, providing evidence for static lithosphere (e.g., Carr 1973).…”

Section: Amazonian Periodmentioning

confidence: 99%

Mars: a small terrestrial planet

Mangold

Baratoux

Witasse

et al. 2016

Astron Astrophys Rev

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Mars is characterized by geological landforms familiar to terrestrial geologists. It has a tenuous atmosphere that evolved differently from that of Earth and Venus and a differentiated inner structure. Our knowledge of the structure and evolution of Mars has strongly improved thanks to a huge amount of data of various types (visible and infrared imagery, altimetry, radar, chemistry, etc) acquired by a dozen of missions over the last two decades. In situ data have provided ground truth for remote-sensing data and have opened a new era in the study of Mars geology. While large sections of Mars science have made progress and new topics have emerged, a major question in Mars exploration-the possibility of past or present life-is still unsolved. Without entering into the debate around the presence of life traces, our review develops various topics of Mars science to help the search of life on Mars, building on the most recent discoveries, going from the exosphere to the interior structure, from the magmatic evolution to the currently active processes, including the fate of volatiles and especially liquid water.

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“…8), which contains one of the youngest lowshield volcanoes and lava flows known on Mars (Plescia 2003;Werner et al 2003;Baratoux et al 2009;Vaucher et al 2009). Because these lava flows and low-shield volcanoes are mostly associated with or originate at the Cerberus Fossae fracture system, which also extends into the Elysium volcanic province, Platz & Michael (2011) argued that both regions share the same magma source at depth.…”

Section: Volcanismmentioning

confidence: 99%

“…Greeley 1974;Greeley & Spudis 1981;Keszthelyi et al 2004), and their derived rheological parameters (e.g. Zimbelman 1985;Baloga et al 2003;Garry et al 2007;Baratoux et al 2009;Hauber et al 2011;Pasckert et al 2012), together with the similarities between terrestrial (e.g. islands of Hawaii and Galapagos) and Martian shield volcanoes (e.g.…”

Section: Composition Of Volcanic Rocksmentioning

confidence: 99%

Volcanism and tectonism across the inner solar system: an overview

Platz

Byrne

Massironi

et al. 2014

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Volcanism and tectonism are the dominant endogenic means by which planetary surfaces change. This book, in general, and this overview, in particular, aim to encompass the broad range in character of volcanism, tectonism, faulting and associated interactions observed on planetary bodies across the inner solar system -a region that includes Mercury, Venus, Earth, the Moon, Mars and asteroids. The diversity and breadth of landforms produced by volcanic and tectonic processes are enormous, and vary across the inventory of inner solar system bodies. As a result, the selection of prevailing landforms and their underlying formational processes that are described and highlighted in this review are but a primer to the expansive field of planetary volcanism and tectonism. In addition to this extended introductory contribution, this Special Publication features 21 dedicated research articles about volcanic and tectonic processes manifest across the inner solar system. Those articles are summarized at the end of this review.

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Shape, rheology and emplacement times of small martian shield volcanoes

Cited by 35 publications

References 34 publications

Acid Rivers and Lakes at Caviahue-Copahue Volcano as Potential Terrestrial Analogues for Aqueous Paleo-Environments on Mars

Acid Rivers and Lakes at Caviahue-Copahue Volcano as Potential Terrestrial Analogues for Aqueous Paleo-Environments on Mars

Mars: a small terrestrial planet

Volcanism and tectonism across the inner solar system: an overview

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