Highs and lows: Using GPR to map cinder cones, lava flows, and lava tubes on Earth to support studies of the Moon and Mars

2020 ◽  
Author(s):  
Sarah Kruse ◽  
Sanaz Esmaeili ◽  
Sajad Jazayeri ◽  
Soraya Alfred ◽  
Ernie Bell ◽  
...  
Keyword(s):  
The Moon ◽  
2021 ◽  
Vol 83 (6) ◽  
Author(s):  
Gianmaria Tortelli ◽  
Anna Gioncada ◽  
Carolina Pagli ◽  
Mauro Rosi ◽  
Laura De Dosso ◽  
...  

AbstractDuring continental rifting, strain and magmatism are believed to localize to narrow magmatic segments, while the rift margin is progressively abandoned. We integrate volcanological, geochemical, petrological and seismic data from the Ma’Alalta volcanic field (MVF) near the western margin of Afar, to show that the MVF is an active magmatic segment. Magmatism in MVF initiated with lava flows and large-volume, caldera-forming ignimbrites from a central edifice. However, the most recent magmatic activity shifted towards mafic lava fields, cinder cones and obsidian-rich silicic domes erupted from vents aligned NNW-SSE, defining a ~ 35-km-long magmatic segment. Along the same area, a NNW-SSE alignment of earthquakes was recorded by two local seismic networks (2005–2009 and 2011–2013). The geochemistry of the mafic rocks is similar to those of nearby axial volcanoes. Inferred magma storage depth from mineral geobarometry shows that a shallow, silicic chamber existed at ~ 5-km depth below the stratovolcano, while a stacked plumbing system with at least three magma storage levels between 9 and 24 km depth fed the recent basalts. We interpret the wide set of observations from the MVF as evidence that the area is an active magmatic segment, showing that localised axial extension can be heavily offset towards the rift margin.


2012 ◽  
Vol 117 (E12) ◽  
pp. n/a-n/a ◽  
Author(s):  
W. B. Garry ◽  
M. S. Robinson ◽  
J. R. Zimbelman ◽  
J. E. Bleacher ◽  
B. R. Hawke ◽  
...  
Keyword(s):  

2017 ◽  
Vol 44 (1) ◽  
pp. 105-112 ◽  
Author(s):  
Loic Chappaz ◽  
Rohan Sood ◽  
Henry J. Melosh ◽  
Kathleen C. Howell ◽  
David M. Blair ◽  
...  
Keyword(s):  
The Moon ◽  

The major factors in the evolution of the lunar surface have not been determined yet. Huge lava flows and lunar differentiation, though commonly assumed, is in discord with much of the evidence. The alternative is for most of the surface to represent the last stages of accretion of the Moon only, with the chemical differentiation having taken place previously in the source material. Radar, seismic, surface exposure, and mascon evidence can then be accounted for. A large-scale surface transport mechanism of soil must then have been present.


2017 ◽  
Vol 44 (20) ◽  
pp. 10,155-10,161 ◽  
Author(s):  
T. Kaku ◽  
J. Haruyama ◽  
W. Miyake ◽  
A. Kumamoto ◽  
K. Ishiyama ◽  
...  
Keyword(s):  
The Moon ◽  

2020 ◽  
Author(s):  
Charlotte Pouwels ◽  
Wieger Wamelink ◽  
Michaela Musilova ◽  
Bernard Foing

<p><strong>Introduction:   </strong>Food demand and the lack of plant nutrients are the main reasons to establish a sustainable agricultural ecosystem on celestial bodies, such as Mars and the Moon. Different kinds of fresh crops, grown in a greenhouse, deliver essential macro and micro nutrients, which have a positive impact on the well-being  of humans. Thus, they will also heavily influence the social interactions of future astronauts. Food development is therefore one of the main activities that will need to be established as soon as possible upon the landing of a human-led mission on another planetary body.</p><p>In addition, crops can be used for air purification and thus oxygen production. Experimental research has been conducted, during a two-week analogue astronaut mission (EMMIHS-II: the second of the EuroMoonMars-IMA-HI-SEAS missions), to grow crops, from garden cress seeds, sown in soil that resembles the regolith on Mars and the Moon. This plant was used because it is easy and fast to grow, which is a priority for research projects during these short-duration missions. In addition, this research will help in reducing compost and fertilizer payloads for upcoming space missions involving human crewmembers.</p><p><strong>Methodology:  </strong>In a remote volcanic region in Hawai’i, United States, the geology and therefore its soil is quite similar to the regolith on Mars and the Moon. For these reasons, the Hawai’i Space Exploration Analog and Simulations (HI-SEAS) habitat was constructed and is being used in this area for space-related research purposes.</p><p>In this habitat, a greenhouse setting had been built with basic requirements for plant growth. The local soil in each of the 70 pots had pre-determined ratio’s with a compost mixture: 0%, 1%, 2%, 3%, 5%, 10%, 25%, 50%, 75%, 100%.  For these settings, the assumption was made that shielding from Solar Energetic Particles (SEP) and Galactic Cosmic Rays (GCR’s) was present. These types of radiation, and thus shielding from the radiation, would be of high relevance on Mars and the Moon to protect the crops there from malformations and death. Future habitats may be located in lava tubes or covered by regolith to address these requirements.</p><p>Here, the presented results focus on the needed ratio of compost to ‘Martian’ simulant soil for garden cress. The results indicate that coarse ‘Martian’ soil with 2% of compost is sufficient for establishing sufficient germination and plant growth in the first stage of plant development. This result leads to promising expectations for other nutrient-soil ratio experiments. In particular for the growth of potatoes and beans, as they are high in nutrients per m<sup>3</sup>.</p><p>Studies on different kinds of soil ratio’s, nutrients delivered per m<sup>3</sup>, radiation shielding and the architecture of an indoor greenhouse setting are of significant relevance to future missions to the Moon and Mars and thus deserve further investigation.</p><p> </p>


2019 ◽  
Vol 9 (1) ◽  
Author(s):  
Ken Ishiyama ◽  
Atsushi Kumamoto

Abstract Elucidation of the subsurface structure in the Smythii basin on the moon is important for understanding lunar volcanic history. Two lava units (Units 1 and 2) cover this basin. The spatial subsurface structure below Unit 2 is unknown. We used SELENE/Lunar Radar Sounder data to identify four subsurface boundaries at 130, 190, 300, and 420 m depths. The radar is reflected at the paleo-regolith layer sandwiched among lava flows, which is supported by a simple radar reflection/transmission model. The spatial distribution of subsurface boundaries demonstrates the deposition of Unit 2 on the subsidence in Unit 1. A simple loading model explained the maximum depth of subsidence (~500 m) and indicated that lithospheric thickness in the Smythii basin was ~24 km at 3.95 Gya. The estimated growth rate of the lithosphere was ~60 km/Ga during 3.95 to 3.07 Gya. After the formation of the Smythii basin at ~4.11 Gya, Unit 1 and Unit 2 deposited with eruption rates of ~8.4 × 10−4 km3/yr by 3.95 Gya and ~7.5 × 10−6 km3/yr by 3.07 Gya respectively. The timing of decline in volcanic activity in the Smythii basin differs from that for the lunar nearside maria, indicating the diversity of volcanism in various lunar areas.


2009 ◽  
Vol 36 (22) ◽  
Author(s):  
Bruce A. Campbell ◽  
B. Ray Hawke ◽  
Lynn M. Carter ◽  
Rebecca R. Ghent ◽  
Donald B. Campbell
Keyword(s):  

Solid Earth ◽  
2019 ◽  
Vol 10 (4) ◽  
pp. 1269-1282 ◽  
Author(s):  
Qiliang Sun ◽  
Christopher A.-L. Jackson ◽  
Craig Magee ◽  
Samuel J. Mitchell ◽  
Xinong Xie

Abstract. Submarine volcanism accounts for ca. 75 % of the Earth's volcanic activity. Yet difficulties with imaging their exteriors and interiors mean that the extrusion dynamics and erupted volumes of deepwater volcanoes remain poorly understood. Here, we use high-resolution 3-D seismic reflection data to examine the external and internal geometry and extrusion dynamics of two late Miocene–Quaternary deepwater (> 2 km emplacement depth) volcanoes buried beneath 55–330 m of sedimentary strata in the South China Sea. The volcanoes have crater-like bases, which truncate underlying strata and suggest extrusion was initially explosive, and erupted lava flows that feed lobate lava fans. The lava flows are > 9 km long and contain lava tubes that have rugged basal contacts defined by ∼90±23 m high erosional ramps. We suggest the lava flows eroded down into and were emplaced within wet, unconsolidated, near-seafloor sediments. Extrusion dynamics were likely controlled by low magma viscosities as a result of increased dissolved H2O due to high hydrostatic pressure and soft, near-seabed sediments, which are collectively characteristic of deepwater environments. We calculate that long-runout lava flows account for 50 %–97 % of the total erupted volume, with a surprisingly minor component (∼3 %–50 %) being preserved in the main volcanic edifice. Accurate estimates of erupted volumes therefore require knowledge of volcano and lava basal surface morphology. We conclude that 3-D seismic reflection data are a powerful tool for constraining the geometry, volumes, and extrusion dynamics of ancient or active deepwater volcanoes and lava flows.


1994 ◽  
Vol 35 (6) ◽  
pp. 1681-1715 ◽  
Author(s):  
M. Z. STOUT ◽  
J. NICHOLLS ◽  
M. A. KUNTZ
Keyword(s):  
The Moon ◽  

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