Methane on Mars: subsurface sourcing and conflicting atmospheric measurements

Oehler, Dorothy Z.; Etiope, Giuseppe

doi:10.1016/b978-0-12-820245-6.00007-0

Cited by 3 publications

(1 citation statement)

References 111 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The minerals of Mars reveal a range of physical and chemical processes that have shaped and modified the red planet over the past 4.5 billion years (Chapman, 2007; Fairén, 2013; Mutch & Arvidson, 1977; Oehler et al., 2021). In many respects, the mineral evolution of Mars mirrors that of Earth and other terrestrial planets and moons (Hazen et al., 2008), with a congruent sequence of primary and secondary formation mechanisms.…”

Section: Introductionmentioning

confidence: 99%

On the Diversity and Formation Modes of Martian Minerals

et al. 2023

View full text Add to dashboard Cite

A systematic survey of 161 known and postulated minerals originating on Mars points to 20 different mineral‐forming processes (paragenetic modes), which are a subset of formation modes observed on Earth. The earliest martian minerals, as on Earth, were primary phases from mafic igneous rocks and their ultramafic cumulates. Subsequent primary igneous minerals were associated with products of limited fractional crystallization, including alkaline and quartz‐normative lithologies. Significant mineral diversification occurred via precipitation of primary phases from aqueous and atmospheric fluids, including authigenesis, hydrothermal and cryogenic precipitation, and evaporites, including freeze drying during eras of low atmospheric pressures. In particular, hydrothermal mineral formation associated with both volcanic fluids and sustained hydrothermal activity in impact fracture zones may have triggered significant mineral diversification, though as yet undocumented. At least 65 such primary minerals have been identified by flown missions to Mars and from martian meteorites. A host of secondary martian minerals were produced by near‐surface processes related to water/rock interactions, including hydration/dehydration, oxidation/reduction, serpentinization, metasomatism, and a variety of diagenetic alterations. Additional mineral diversity resulted from metamorphic events, including thermal and shock metamorphism, lightning, and bolide impacts. However, several dominant sources of mineral diversity on Earth, including: (1) extensive fluid/rock interactions and element concentration associated with plate tectonics; (2) high‐pressure regional metamorphism associated with plate tectonics; and (3) biologically mediated mineralization—are not known to be in play on Mars. Consequently, we estimate the total mineral diversity of Mars to be an order of magnitude smaller than on Earth.

show abstract

Section: Introductionmentioning

confidence: 99%

On the Diversity and Formation Modes of Martian Minerals

et al. 2023

View full text Add to dashboard Cite

show abstract

A review of the meteor shower hypothesis for methane on Mars

Fries

2021

Mars Geological Enigmas

View full text Add to dashboard Cite

An overview of sedimentary volcanism on Mars

Brož¹,

Oehler²,

Mazzini³

et al. 2023

Earth Surf. Dynam.

View full text Add to dashboard Cite

Abstract. Extensive fields of sub-kilometre- to kilometre-scale mounds, cones, domes, shields, and flow-like edifices cover large parts of the martian lowlands. These features have been compared to structures on Earth produced by sedimentary volcanism – a process that involves subsurface sediment/fluid mobilisation and commonly releases methane to the atmosphere. It was proposed that such processes might help to explain the presence of methane in the martian atmosphere and may also have produced habitable, subsurface settings of potential astrobiological relevance. However, it remains unclear if sedimentary volcanism on Earth and Mars share genetic similarities and hence if methane or other gases were released on Mars during this process. The aim of this review is to summarise the current knowledge about mud-volcano-like structures on Mars, address the critical aspects of this process, identify key open questions, and point to areas where further research is needed to understand this phenomenon and its importance for the Red Planet's geological evolution. We show here that after several decades of exploration, the amount of evidence supporting martian sedimentary volcanism has increased significantly, but as the critical ground truth is still lacking, alternative explanations cannot be ruled out. We also highlight that the lower gravity and temperatures on Mars compared to Earth control the dynamics of clastic eruptions and surface emplacement mechanisms and the resulting morphologies of erupted material. This implies that shapes and triggering mechanisms of mud-volcano-like structures may be different from those observed on Earth. Therefore, comparative studies should be done with caution. To provide a better understanding of the significance of these abundant features on Mars, we argue for follow-up studies targeting putative sedimentary volcanic features identified on the planet's surface and, if possible, for in situ investigations by landed missions such as that by the Zhurong rover.

show abstract

Methane on Mars: subsurface sourcing and conflicting atmospheric measurements

Cited by 3 publications

References 111 publications

On the Diversity and Formation Modes of Martian Minerals

On the Diversity and Formation Modes of Martian Minerals

A review of the meteor shower hypothesis for methane on Mars

An overview of sedimentary volcanism on Mars

Contact Info

Product

Resources

About