Analysis of Lava Tubes and Skylights in the Lunar Exploration Context
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Aitken Basin
Geological and geochemical analysis of units in the South Pole – Aitken Basin A.M. Borst¹,², F.S. Bexkens¹,², B. H. Foing², D. Koschny² ¹ Department of Petrology, VU University Amsterdam ² SCI-S. Research and Scientific Support Department, ESA – ESTEC Student Planetary Workshop 10-10-2008 ESA/ESTEC The Netherlands The South Pole – Aitken Basin Largest and oldest Lunar impact basin - Diameter > 2500 km - Depth > 12 km - Age 4.2 - 3.9 Ga Formed during Late heavy bombardment? Window into the interior and evolution of the Moon Priority target for future sample return missions Digital Elevation Model from Clementine altimetry data. Produced in ENVI, 50x vertical exaggeration, orthographic projection centered on the far side. Red +10 km, purple/black -10km. (A.M.Borst et.al. 2008) 1 The Moon and the SPA Basin Geochemistry Iron map South Pole – Aitken Basin mafic anomaly • High Fe, Th, Ti and Mg abundances • Excavation of mafic deep crustal / upper mantle material Thorium map Clementine 750 nm albedo map from USGS From Paul Lucey, J. Geophys. Res., 2000 Map-a-Planet What can we learn from the SPA Basin? • Large impacts; Implications and processes • Volcanism; Origin, age and difference with near side mare basalts • Cratering record; Age, frequency and size distribution • Late Heavy Bombardment; Intensity, duration and origin • Composition of the deeper crust and possibly upper mantle 2 Topics of SPA Basin study 1) Global structure of the basin (F.S. Bexkens et al, 2008) • Rims, rings, ejecta distribution, subsequent craters modifications, reconstructive -
Geologic Structure of Shallow Maria
NASA CR. Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator John A. Waskom, Co-Investigator (NASA-CR-lq7qoo GEOLOGIC STahJCTUnF OF N76-17001 ISBALOW M1BIA-'(Arkansas Uni.v., mHiticelio.) 96 p BC $5.00' CSCL O3B Unclas G3/91, 09970- University of Arkansas at Monticello Monticello, Arkansas December 1975 Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator I John A. Waskom, Co-Investigator Un-iversity-of Arkansas-:at-.Monticl o Monticello, Arkansas December 1975 ABSTRACT Isopach maps and structural contour maps of the 0 0 eastern mare basins (30 N to 30 OS; 00 to 100 E) are constructed from measurements of partially buried craters. The data, which are sufficiently scattered to yield gross thickness variations, are restricted to shallow maria with less than 1500-2000 m of mare basalts. The average thickness of b-asalt in the irregular maria is between 200 and 400 m. Multiringed mascon basins are filled to various levels. The Serenitatis and Crisium basins have deeply flooded interiors and extensively flooded shelves. Mare basalts in the Nectaris basin fill only the innermost basin, and mare basalts in the Smythii basin occupy a small portion of the basin floor. Sinus Amoris, Mare Spumans, and Mare Undarum are partially filled troughs concentric to large circular basins. The Tranquillitatis and Fecunditatis are composite depressions containing basalts which flood degraded circular basins and adjacent terrain modified by the formation of nearby cir cular basins. -
EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 C Author(S) 2011
EPSC Abstracts Vol. 6, EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 Analysis of mineralogy of an effusive volcanic lunar dome in Marius Hills, Oceanus Procellarum. A.S. Arya, Guneshwar Thangjam, R.P. Rajasekhar, Ajai Space Applications Centre, Indian Space Research Organization, Ahmedabad-380 015 (India). Email:[email protected] Abstract found on the lunar surface. As a part of initiation of the study of mineralogy of MHC, an effusive dome Domes are analogous to the terrestrial shield located in the south of Rima Galilaei, near the volcanoes and are among the important volcanic contact of Imbrian and Eratosthenian geological units features found on the lunar surface indicative of is taken up for the present study. The morphology, effusive vents of primary volcanism within Mare rheology and the possible dike parameters have regions. Marius Hills Complex (MHC) is one of the already been studied and reported [5]. most important regions on the entire lunar surface, having a complex geological setting and largest distribution of volcanic constructs with an abundant number of volcanic features like domes, cones and rilles. The mineralogical study of an effusive dome located in the south of Rima Galilaei, near the contact of Imbrian and Eratosthenian geological units is done using hyperspectral band parameters and spectral plots so as to understand the compositional variation, the nature of the volcanism and relate it to the rheology of the dome. Fig. 1: Distribution of dome in MHC (Red-the dome under study, Green- from Virtual Moon Atlas, Magenta [6]) and the Study area showing the dome under study on M3 1. -
Mare Domes in Mare Tranquillitatis: Identification, Distribution, Characteristics, and Implications for Their Origin and the Oldest Lunar Volcanism
51st Lunar and Planetary Science Conference (2020) 1798.pdf MARE DOMES IN MARE TRANQUILLITATIS: IDENTIFICATION, DISTRIBUTION, CHARACTERISTICS, AND IMPLICATIONS FOR THEIR ORIGIN AND THE OLDEST LUNAR VOLCANISM. L. Qiao1, J. W. Head2, L. Wilson3 and Z. Ling1, 1Inst. Space Sci., Shandong Univ., Weihai, Shan- dong, 264209, China ([email protected]), 2Dep. Earth, Env. & Planet. Sci., Brown Univ., Providence, RI, 02912, USA, 3Lancaster Env. Centre, Lancaster Univ., Lancaster LA1 4YQ, UK. Introduction: Volcanism is one of the major geo- General Characteristics and Identification Crite- logical process on the Moon, directly reflecting the ria of Mare Domes. A preliminary survey of previous- composition and thermal state of lunar interior and its ly-catalogued mare domes [1-4] reveals some of their evolution, and serves as an important window into the fundamental characteristics. A typical well-developed geological and thermal evolution of the Moon. Mare mare dome is characterized by a domical raised struc- domes, small (<~30 km diameter) and generally circu- ture with a generally convex-shape and low-slope (<5°) lar structures with convex-upward shapes [1], are profile and a (quasi-)circular or elliptical outline. Some among the most common volcanic landforms on the domes have summit pit craters, while many lack them, Moon. Over 300 mare domes have been previously possibly being filled up by the last eruptions. The de- identified, using mainly telescope and orbital photo- velopment of the circular mound shape of mare domes graphs [e.g., 1-4]. -
ANTIPODES on the MOON J.F.Rodionova, E.A.Kozlova
Lunar and Planetary Science XXXI 1349.pdf ANTIPODES ON THE MOON J.F.Rodionova, E.A.Kozlova Sternberg State Astronomical Institute, Russia Laser altimetry data from accidental coincidence of the antipodes Clementine has allowed to determine is very little (4). some of nearly obliterated multiring The aim of the paper is an basins on the Moon that could not be attempt to reveal antipodes for the new determined on the basis of previous basins detected by the Clementine surveying. The Mendel-Rydberg altimetry. The fact is that the Mutus- Basin, a degraded three ring feature Vlacq Basin is the antipode of the with 630 km in diameter to the south Birkhoff Basin and Friendlich- of Mare Orientale is about 6 km deep Sharonov is the antipode of Mare from rim to floor (1). The Coulomb- Nubium. The detailed data of the all Sarton Basin has been discovered on revealed antipodes is given in Fig. 1.. the northwestern portion of the lunar There is no antipode for the Coulomb- far side. Clementine altimetry reveals a Sarton Basin, but there is Rheita Vallis basin about 490 km in diameter on its place. averaging 6 km in depth, rim to floor. The real nature of the antipodes Tree basins in diameter more than 600 is not clear now. The possibility of km were revealed in the neighbour of convergence of the waves in the the craters Freundlich-Sharonov, antipodal point of the impact is Tsiolkovskiy-Stark, Lomonosov- discussed in some papers. Schults and Fleming. The Mutus-Vlacq Basin an Gault (5) consider that formation of ancient feature on the near side was large basin on the terrestrial planets detected by the altimetry. -
A Guideline for a Sustainable Lunar Base Design for Constructed in Lunar Lava Tubes and Their Vertical Skylights
50th International Conference on Environmental Systems ICES-2021-186 12-15 July 2021 A Guideline for a Sustainable Lunar Base Design for Constructed in Lunar Lava Tubes and Their Vertical Skylights Masato Sakurai1, Asuka Shima2, Isao Kawano3, Junichi Haruyama4 Japan Aerospace Exploration Agency (JAXA), Chofu-shi, Tokyo, 182-8522, Japan. and Hiroyuki Miyajima5 International University of Health and Welfare, Narita Campus 1, 4-3, Kōzunomori, Narita, Chiba, 286-8686 Japan The lunar surface is a hostile environment subject to harmful radiation and meteorite impacts. A recently discovered lava tube avoids these risks and, as it undergoes only slight temperature changes, it is a promising location for constructing a lunar base. JAXA engages in research in regenerative ECLSS (Environmental Control Life Support Systems), particularly addressing water and air recycling and treating organic waste. Overcoming these challenges is essential for long-term lunar habitation. This paper presents a guideline for a sustainable lunar base design. Nomenclature ECLSS = Environmental Control Life Support System HTV = H-II Transfer Vehicle ISS = International Space Station JAXA = Japan Aerospace Exploration Agency JSASS = Japan Society for Aeronautical and Space Science MHH = Marius Hills Hole MIH = Mare Ingenii Hole MTH = Mare Tranquillitatis Hole SELENE = Selenological and Engineering Explorer UZUME = Unprecedented Zipangu Underworld of the Moon Exploration (name of the research group for vertical holes) SDGs = Sustainable Development Goals SELENE = Selenological and Engineering Explorer I. Introduction uture space exploration will extend beyond low Earth orbit and dramatically expand in scope. In particular, F industrial activities are planned for the Moon with the development of infrastructure that includes lunar bases. This paper summarizes our study of the construction of a crewed permanent settlement, which will be essential to support long-term habitation, resource utilization, and industrial activities on the Moon. -
The Moon After Apollo
ICARUS 25, 495-537 (1975) The Moon after Apollo PAROUK EL-BAZ National Air and Space Museum, Smithsonian Institution, Washington, D.G- 20560 Received September 17, 1974 The Apollo missions have gradually increased our knowledge of the Moon's chemistry, age, and mode of formation of its surface features and materials. Apollo 11 and 12 landings proved that mare materials are volcanic rocks that were derived from deep-seated basaltic melts about 3.7 and 3.2 billion years ago, respec- tively. Later missions provided additional information on lunar mare basalts as well as the older, anorthositic, highland rocks. Data on the chemical make-up of returned samples were extended to larger areas of the Moon by orbiting geo- chemical experiments. These have also mapped inhomogeneities in lunar surface chemistry, including radioactive anomalies on both the near and far sides. Lunar samples and photographs indicate that the moon is a well-preserved museum of ancient impact scars. The crust of the Moon, which was formed about 4.6 billion years ago, was subjected to intensive metamorphism by large impacts. Although bombardment continues to the present day, the rate and size of impact- ing bodies were much greater in the first 0.7 billion years of the Moon's history. The last of the large, circular, multiringed basins occurred about 3.9 billion years ago. These basins, many of which show positive gravity anomalies (mascons), were flooded by volcanic basalts during a period of at least 600 million years. In addition to filling the circular basins, more so on the near side than on the far side, the basalts also covered lowlands and circum-basin troughs. -
GRAIL-Identified Gravity Anomalies In
Solar System Exploration Division, GSFC Code 690 GRAIL-identified gravity anomalies in Oceanus Procellarum: Insight into subsurface impact and volcanic/magmatic structures on the Moon Ariel N. Deutsch1, Gregory A. Neumann2, James W. Head1 1Department of Earth, Environmental and Planetary Sciences, Brown University, 2NASA Goddard Space Flight Center Introduction: Lunar gravity anomalies. Positive Bouguer gravity anomalies. • Four distinctive positive Bouguer gravity anomalies are • Previous work has suggested that these four positive gravity anomalies may be due to: -Subsurface volcanic sills [2]. • New, higher-resolution GRAIL data [3] allow for the re- analysis of these anomalies. • Understanding the subsurface density structures that contribute to these anomalies is important in order to discuss regional impact and volcanic histories, and the evolution of the lunar crust in Oceanus Procellarum. Objectives. 1. Constrain subsurface structures that contribute to the . four positive Bouguer gravity anomalies. 2. Discuss the hidden impact and volcanic histories of . the Moon. Methods. Results: Filled and buried impact craters. RESULTS: MANTLE UPWELLING • Six geologic end-member scenarios are explored to 20 200 1. Filled and Buried Impact 2. Southern Aristarchus Plateau analyze the four observed gravitational anomalies. 15 Model 3 10 GRAIL 100 • Impact crater parameters [e.g., 4] are estimated to C Gravity 5 B from uplift Gravity from A 0 0 km -3 km km ρ = 3150 kg m -5 mGal mGal • Analyses of the generation, ascent, and eruption of -3 mGal ρ = 2800 kg m crater -10 Surface topography -100 -3 of subsurface magmatic structures and also the . -15 ∆ρ = 600 kg m Highland crust -20 -200 Mantle interpretation of surface volcanic features. -
Geological Evolution of the Largest Shield Volcano Bearing Mare of The
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1827.pdf GEOLOGICAL EVOLUTION OF THE LARGEST SHIELD VOLCANO BEARING MARE OF THE MOON, MARE TRANQUILLITATIS: BASED ON DETAILED MORPHOLOGICAL, MINERALOGICAL, TOPOGRAPHIC STUDIES USING MULTIPLE DATA SETS. Henal Bhatt1, P. Chauhan2, Paras Solanki1, 1M. G. Science Institute, Ahmedabad 380009, India, 2Indian Institute of Remote Sensing, (ISRO), Dehradun, Uttarakhand, India. ([email protected] ) Introduction: In this work, we have analysed the Results and Discussions: Mare Tranquillitatis is irregular shaped Mare Tranquillitatis based on its delineated in to 22 spectral units based on IBD parameter morphology, mineralogy and topography to understand its analysis (Fig. 1). The band parameters analysis was geological evolution in the Lunar formation history. This conducted as per [8], [9], [10] suggest the abundance of area is very unique as it resides the largest shield volcano mafic silicate mixture, particular, mixture of olivine and of the Moon, compared to all the other circular mare basins medium to high calcium pyroxene bearing basaltic material at the near side of the Moon. It is located towards eastern in the area (Fig. 1). Details of this analysis is reported in the near side at 7°N, 30°E and is a Pre-Nectarian age basin [1]. [11]. Graphical trends suggests that basalts of eastern shield It is well known for Apollo 11 landing site and it shows mare would have been comparatively more pyroxene characteristic two basin ring structure [2], with diameter of bearing compared to the basalts from western deepest part, 800 km from east to west. which would have been more olivine bearing compared to the eastern shield mare basalt (Fig. -
To the Moon and Back - Weighing for NASA
To the Moon and Back - Weighing for NASA A small step carrying a lot of weight: The 1969 lunar landing. It sent TV viewer ratings rocketing into the stratosphere and drove innumerable companies and universities to extraordinary accomplishments. The objective: To ensure the success of the Apollo II mission. Mettler Instrument Corporation was one of the companies that supported NASA. This collaboration is still alive and well. "The eagle has landed!" Those are the words Neil Alden Armstrong transmitted back to the space administration on July 20, 1969. Shortly before, he planted the Eagle lunar module in the Mare Tranquillitatis, the "Sea of Tranquility". A long journey for the astronauts of the Apollo II mission - the average distance from the Earth to the moon is about sixty-times around the world, or about 384,401 kilometers. Mission commander Armstrong and Edwin "Buzz" Aldrin move about like feather weights on the powdery surface of earth's orbiter. Instead of the 360 pounds on Earth, their suits weigh only 60 pounds because of Moon's gravity, which is only one-sixth that of the Earth. Space exploration and Apollo mission Meanwhile, Michael Collins, the third Apollo II astronaut, orbits the moon in the space ship and shoots the pictures that on the next day are circulating around the world: They show the Eagle lunar module on its return voyage from the lunar surface to the mother ship. Around 400,000 people and 20,000 companies and universities worldwide supported the Apollo program at its height. Among them was Mettler Instrument Corporation of Greifensee near Zurich. -
Glossary of Lunar Terminology
Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites. -
Lunar Pits Gateway to the Subsurface Mark Robinson and Robert Wagner Outline
Lunar Pits Gateway to the Subsurface Mark Robinson and Robert Wagner Outline • Overview of pits • Good destinations • Arne mission Pits: What are they? • Small, steep-walled collapse features • Of >300 known, all but 16 in impact melts Pits are widespread on the Moon White: Mare and highland pits Blue: Impact melt pits Pits are widespread on the Moon White: Mare and highland pits Blue: Impact melt pits Pits are interesting for exploration • Exposed layer profiles • Benign environment • Radiation, meteorites, temperature variation • Potential cave access • Access to un[space]weathered minerals Top panels from Robinson et al. 2012 Bottom-right from Daga and Daga 1992 Desired data from initial visit • cm-scale wall and floor morphology/albedo • Stretch goal: Composition of layers • Thermal and radiation environment • Presence and extent of any caves • Traversibility Top panels from Robinson et al. 2012 Bottom-right from Daga and Daga 1992 Pit Exploration Challenges • Probably can’t just “drive up to the rim” and see the floor • Surrounding “funnels” are likely unstable • Need a tether or flight • Limited lighting within • Difficult to communicate out Top: Devil’s Throat in Hawai‘i Bottom: Oblique view of Mare Ingenii pit Good targets for exploration Good targets for exploration • Mare Ingenii • 100 x 68 x 65 m • Large overhung region on west side (>20 m) • On lunar far side Good targets for exploration • Lacus Mortis • >150 x 110 x 80 m • 23° entrance slope, • Almost certainly no caves Good targets for exploration • Marius Hills • 58 x 49