Volcanism and tectonism across the inner solar system: an overview

Platz, Thomas; Byrne, P. K.; Massironi, Matteo; Hiesinger, H.

doi:10.1144/sp401.22

Cited by 49 publications

(10 citation statements)

References 473 publications

(608 reference statements)

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“…Conversely, Martian plume-fed edifices have remained connected to their magma sources for extraordinary lengths of time—in some cases for billions of years 5 , 7 , 8 . As a consequence, although morphologically similar to shield volcanoes on Earth, Martian volcanoes have grown to be the largest in the solar system 9 (Fig. 1 ).…”

Section: Introductionmentioning

confidence: 99%

Taking the pulse of Mars via dating of a plume-fed volcano

et al. 2017

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Mars hosts the solar system’s largest volcanoes. Although their size and impact crater density indicate continued activity over billions of years, their formation rates are poorly understood. Here we quantify the growth rate of a Martian volcano by 40Ar/39Ar and cosmogenic exposure dating of six nakhlites, meteorites that were ejected from Mars by a single impact event at 10.7 ± 0.8 Ma (2σ). We find that the nakhlites sample a layered volcanic sequence with at least four discrete eruptive events spanning 93 ± 12 Ma (1416 ± 7 Ma to 1322 ± 10 Ma (2σ)). A non-radiogenic trapped 40Ar/36Ar value of 1511 ± 74 (2σ) provides a precise and robust constraint for the mid-Amazonian Martian atmosphere. Our data show that the nakhlite-source volcano grew at a rate of ca. 0.4–0.7 m Ma−1—three orders of magnitude slower than comparable volcanoes on Earth, and necessitating that Mars was far more volcanically active earlier in its history.

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Section: Introductionmentioning

confidence: 99%

Taking the pulse of Mars via dating of a plume-fed volcano

et al. 2017

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“…By contrast, an abundance of impact structures are preserved on solid solar system bodies lacking significant tectonics and resurfacing, such as Mercury and the Moon. Their study is limited by the current observational means, and models draw heavily on topographic‐feature analysis and information from spectral data [ Platz et al ., ]. The small number of well‐preserved terrestrial impact sites and the scarcity of in situ geological data for the nonterrestrial impact basins conspire to significantly limit the knowledge regarding the potential for large impacts to rework or destroy the impacted lithosphere [e.g., Moser et al ., ].…”

Section: Introductionmentioning

confidence: 99%

Protracted volcanism after large impacts: Evidence from the Sudbury impact basin

et al. 2017

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Morphological studies of large impact structures on Mercury, Venus, Mars, and the Moon suggest that volcanism within impact craters may not be confined to the shock melting of target rocks. This possibility prompted reinvestigation of the 1.85 Ga subaqueous Sudbury impact structure, specifically its 1.5 km thick immediate basin fill (Onaping Formation). Historically, breccias of this formation were debated in the context of an endogenic versus an impact‐fallback origin. New field, petrographic, and in situ geochemical data document an array of igneous features, including vitric shards, bombs, sheet‐like intrusions, and peperites, preserved in exquisite textural detail. The geochemistry of vitric materials is affected by alteration, as expected for subaqueous magmatic products. Earlier studies proposed an overall andesitic chemistry for all magmatic products, sourced from the underlying impact melt sheet. The new data, however, suggest progressive involvement of an additional, more magnesian, and volatile‐rich magma source with time. We propose a new working model in which only the lower part of the Onaping Formation was derived by explosive “melt‐fuel‐coolant interaction” when seawater flooded onto the impact melt sheet in the basin floor. By contrast, we suggest that the upper 1000 m were deposited during protracted submarine volcanism and sedimentary reworking. Magma was initially sourced from the impact melt sheet and up stratigraphy, from reservoirs at greater depth. It follows that volcanic deposits in large impact basins may be related to magmatism caused by the impact but not directly associated with the impact‐generated melt sheet.

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“…Might Venus's atmospheric evolution be episodic, with multiple overturn and volcanic recycling events in its history (e.g., Armann & Tackley, ; Moresi & Solomatov, ; Strom et al, )? Does the current surface temperature and environment influence the style of tectonics through deeply penetrating thermal effects (Ghail, ; Platz et al, )? Perhaps, examples of these separate and divergent evolutionary paths are present in the cornucopia of discovered Venus‐like exoplanets.…”

Section: The Geological Enigmamentioning

confidence: 99%

Venus as a Laboratory for Exoplanetary Science

Kane

Arney²,

Crisp

et al. 2019

JGR Planets

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The current goals of the astrobiology community are focused on developing a framework for the detection of biosignatures, or evidence thereof, on objects inside and outside of our solar system. A fundamental aspect of understanding the limits of habitable environments (surface liquid water) and detectable signatures thereof is the study of where the boundaries of such environments can occur. Such studies provide the basis for understanding how a once inhabitable planet might come to be uninhabitable. The archetype of such a planet is arguably Earth's sibling planet, Venus. Given the need to define the conditions that can rule out bio‐related signatures of exoplanets, Venus provides a unique opportunity to explore the processes that led to a completely uninhabitable environment by our current definition of the term. Here we review the current state of knowledge regarding Venus, particularly in the context of remote‐sensing techniques that are being or will be employed in the search for and characterization of exoplanets. We discuss candidate Venus analogs identified by the Kepler and TESS exoplanet missions and provide an update to exoplanet demographics that can be placed in the potential runaway greenhouse regime where Venus analogs are thought to reside. We list several major outstanding questions regarding the Venus environment and the relevance of those questions to understanding the atmospheres and interior structure of exoplanets. Finally, we outline the path toward a deeper analysis of our sibling planet and the synergy to exoplanetary science.

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Volcanism and tectonism across the inner solar system: an overview

Cited by 49 publications

References 473 publications

Taking the pulse of Mars via dating of a plume-fed volcano

Taking the pulse of Mars via dating of a plume-fed volcano

Protracted volcanism after large impacts: Evidence from the Sudbury impact basin

Venus as a Laboratory for Exoplanetary Science

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