DOCSLIB.ORG

Composition Analysis of the Marius Hills Volcanic Complex Using Diviner Lunar Radiometer Experiment and Moon Mineralogy Mapper

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Composition Analysis of the Marius Hills Volcanic Complex Using Diviner Lunar Radiometer Experiment and Moon Mineralogy Mapper 44th Lunar and Planetary Science Conference (2013) 1225.pdf Composition Analysis of the Marius Hills Volcanic Complex using Diviner Lunar Radiometer Experiment and Moon Mineralogy Mapper. K. M. Lehman1,2 , G. Y. Kramer2, R. G. Mayne1,3, W. S. Kiefer2, 1School of Geology, Energy, and the Environment, Texas Christian University, Fort Worth, TX ([email protected]), 2Lunar and Planetary Institute, Houston, TX. 3Monnig Meteorite Gallery, Fort Worth, TX. Introduction: the material [9, 10]. It is also important to note that a low CF value has a high correlation to high visual al- The Marius Hills Volcanic Complex, located in bedo, and that space weathering causes the CF value to Central Oceanus Procellarum at 13.3 N, 306.8 E , has move to longer wavelengths [10, 11]. All this makes an undoubtedly complicated volcanic history. Over 250 domes and complex surrounding volcanic geo- the CF value very helpful in understanding the geology morphologies suggest multiple volcanic episodes[1]. In of an area. This value is complementary to M3 spectra, allowing for more felsic materials to be observed and light of this, many have investigated potential compo- for a deeper understanding of the entire compositional sitional differences using both Clementine and Chan- mixture as comparison between spectra compositions dryann-1’s Moon Mineralogy Mapper (M3 ) and have and Diviner compositions occur. identified the area as a high titanium basalt with glass features surrounding cones associated with pyroclastic Methodology: [2,3,4]. Beyond subtle variation in FeO percent, TiO2 Three different data sets were used to analyze percent and olivine content, the complex has been this region: Clementine, M3 spectral data, and the deemed compositionally homogenous [2,3,5]. Recent Gridded Level 3 Diviner Christiansen Feature map. geophysical research has shown a large gravity anoma- ly under the Marius Hills complex that can be best We initially used RGB (Band-Ratio Color Com- explained by a large magma chamber, large enough to posite) [12], TiO2 [13], FeO [14] spectral image maps allow for significant magma evolution [6]. This new from the 5 channel UV VIS imager on the Clementine evidence made it important to analyze possible compo- spacecraft. We also used M3 data to create spectral sitional differences using data sets that have not been parameter maps, that were designed to highlight re- used before. gions that are rich in particular materials such as oli- vine and high calcium pyroxene. The M3 maps were Our study makes use of two complementary spec- overlaid on to the Clementine data to differentiate tral datasets. M3 is an imaging reflectance spectrometer chemically different areas. These areas were then ana- that can detect 85 channels between 460 to 3000 nm, lyzed using the M3 spectral profiles to see if there and has a spatial resolution of 140 meter per pixel [7]. were actual notable changes in the spectra. We particu- M3 can determine mineralogy in reflectance spectra larly focused on looking for possible spectral differ- through diagnostic absorptions at specific wavelengths, ences between the Marius Hills volcanic domes and which result from electronic transitions between an the lava plains between the domes. Based on the geo- iron atom and its surrounding oxygens in a crystal logic regions mapped out using these parameters we structure [8]. The specific wavelengths at which these extracted representative M3 spectra for more detailed absorptions occur are dictated by the composition and spectral analysis. crystal structure of a specific mineral. M3 is particular- ly effective at detecting pyroxene and olivine, but can We also looked for possible differences in the lo- only detect plagioclase when it is verypure. Previous cation of Christiansen absorption frequency using Di- analysis of the near infrared spectrum of the Marius viner radiometer results[9, 10]. Areas that displayed Hills used a preliminary calibration of M3 spectroscopy differences were then compared with their M3 spectral [5], whereas our analysis uses the final calibration of counterparts to see if there was a correlation between the M3 dataset. the two data sets. Finally, Lunar Reconnaissance Or- The Lunar Reconnaissance Orbiter’s (LRO) Di- biter Camera (LROC) and WAC GLD 100 stereo to- viner Lunar Radiometer Experiment has a spatial reso- pography model were used to try to understand the lution of 950 m/pixel [10]. Diviner produces thermal geomorphology of the areas that appeared chemically emissivity data, and can provide compositional infor- different. mation from 3 wavelengths centered around 8 microns M3 Analysis: that are used to characterize the Christiansen Feature (CF) [9, 10]. Each CF value is indicative of a certain The analysis of the Marius Hills complex us- silicate mineral composition, with higher values being ing the most recent M3 calibration bears similar results a more mafic material and lower values being felsic [9, to previous studies. The complex appears relatively 10]. This feature is not affected by vitrification and the homogenous spectrally, with variations only seen in value can be assumed to be based on linear mixing of the absorption band depths and the reddening (ma- 44th Lunar and Planetary Science Conference (2013) 1225.pdf recent M3 calibration. muted pyroxene absorptions and a brightening of the Plagioclase rich areas spectra. 0.2 Pyroxene rich areas Discussion 0.15 3 The new Diviner data shows what M could 0.1 not alone, plagioclase rich regions in the Marius Hills complex. Mineral components that combine to form 0.05 reflectance spectra do not mix linearly at modal abun- dances as low as 10 percent strongly absorbing dark 0 minerals, such as olivine, pyroxene, ilmenite, can Apparent Reflectance 0.5 1.5 2.5 3.5 overwhelm and obscure a plagioclase spectrum [10]. Wavelength (micron) Bright craters and bright areas surrounding domes in the NAC images which are associated with low CF Plagioclase rich areas values are assumed to be the plagioclase-rich areas. 1.30 Pyroxene rich areas These bright, plagioclase rich areas, are often sur- 1.20 rounded by very low albedo which may be more il- 1.10 menite rich materials. 1.00 0.90 Reflectance 0.80 Figure 2: This map, which has a WAC image overlaid by a Continuum Removed 0.70 color relief map based on WAC GLD 100 topography as its 0.5 1.0 1.5 2.0 2.5 3.0 3.5 base, displays the plagioclase rich domes. The 8 major domes Wavelength (micron) that are observed as plagioclase rich by the Diviner Lunar Radiometer Experiment are outlined in heavy black. FigureFigure 1: These 1: These graph graph displays displays the the difference difference betweenbetween the the PlagioclasePlagioclase rich rich areas areas (purple) (purple) andand thethe surrounding surrounding non plnonplagia- o- gioclase rich areas (blue). Top: Raw spectra Bottom: Continu- clase-umrich Removed areas (blue).spectra. Top:Removing Raw the spectra continuum Bottom: slope from Continuum the Removedtop spectra spectra. em phasizesRemoving the relativethe continuum strength of slope the 1 fromand 2 the top mciron absorbtions for pyroxene. As can be seen, the Plagio- Discussion: spectraclase em richphasizes areas are the brighter relative with strength muted absorptions. of the 1 and 2 micron absor ptions for pyroxene. As can be seen, the Plagioclase-rich Figure 2: This map,The which new has aD WACivin imageer data overlaid reveals by a col theor presence of areas areDiviner brighter Analysis with muted absorptions. relief map based on WAC GLD 100 topography as its base, Previous studies have used Diviner data to displays theplagi plagioclaseoclase rich- richdomes. regions The 8 major within domes thatthe are Ma rius Hills. This map more silica rich areas on the moon, but none of observed as plagioclase rich by the Diviner Lunar Radiometer Experimentconclusion are outlined in heavywas black.not possible using M3 data, because turity)these of thehave spectra. focused Ason theseen Marius in Figure Hills Complex 1, the spectra [9, display10]. classic Although pyroxene the area had absorptions, an average CF primarily value of 8.3 that of strong absorptions from even small abundances of py- microns suggesting a pyroxene rich substance, there Remoteroxene sensing and olivine observations overwhelm show that the the weak near-infrared clinopyroxene,are areas across with the its complex 1 and that 2 micronhave CF absorvalues prantionsg- Marius Hills basalts are relatively high in Ti [17]. ing 7.9- 8.2 microns suggesting a more plagioclase rich Based onabsorption this, we use ofApollo plagioclase 17 high titanium [ 16]. Brightbasalt craters and shiftedarea. to longerThese plagiwavelengthsoclase regions [15]. are Previous associated studieswith 70215 as an analog for the crystallization of the Marius had describedmany craters, an rilles, olivine possible rich vo flowlcanic within vents and the with co m8 plexHills basalts.bright Petrographic areas surrounding observations domes and exper in thei- NAC images large domes. The largest of these lower CF value mental crystallizationwhich are studiesassocia showted thatwith the low major CF mi valuesn- are assumed [5], butdomes we isdid made not upsee of this 65 divinervariation pixels using covering the mostap- erals in 70215 began crystallizing in the following or- recentproximately M3 calibr 62a tion.km2. For each roughly km sized pixel, der: olivine,to beilmenite, the plagioclase and then pyroxene-rich areas. and plagi Theseo- bright, plagio- the CF value, and thus the composition, can be as- clase appearedclase
Load more

Recommended publications
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • Analysis of Lava Tubes and Skylights in the Lunar Exploration Context
    EPSC Abstracts Vol. 7 EPSC2012-632-1 2012 European Planetary Science Congress 2012 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2012 Analysis of Lava Tubes and Skylights in the Lunar Exploration Context E. Martellato, B. Foing, J. Benkhoff ESA/ESTEC, Keplerlaan 1, 2201 Noordwijk ZH, The Netherlands (corresponding author: [email protected], [email protected]) collapsed sections of roofs ([6]). Skylights could Abstract originate as enlargement of pre-existing fractures, for instance following a moonquake ([8]), or as The past and current scientific activities related to the incompleting crusting over the melted lava flow (e.g., future robotic and human exploration of the Moon [4]), or as collapse of the lava tubes ceiling caused by have stressed the importance of lava tubes as random meteoroids impacts (e.g., [6]). convenient settlements in an inhospitable planet, providing a natural shielding to a variety of natural 2. Observations hazards with minimizing costs of the construction of manned bases. The detection of lava tubes could be In our analysis, we consider two skylights candidates favoured by the presence of skylights, which also detected by the Terrain Camera onboard the Japanese represent a way to access to these underground orbiter SELenological and Engineering Explorer structures. In this context, we analyze one of the (SELENE) ([9], [10]), and then observed at higher proposed mechanism of skylights formation, that is resolution by Lunar Reconnaissance Orbiter Camera random impacts craters, by comparing crater- (LROC) onboard the NASA spacecraft Lunar geometry argumentations ([11]) with numerical Reconnaissance Orbiter (LRO) ([2]). modelling outcomes. A first pit is located on the Marius Hills region 1.
    [Show full text]
  • 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.
    [Show full text]
  • GRAIL-Identified Gravity Anomalies in Oceanus Procellarum: Insight Into 2 Subsurface Impact and Magmatic Structures on the Moon 3 4 Ariel N
    1 GRAIL-identified gravity anomalies in Oceanus Procellarum: Insight into 2 subsurface impact and magmatic structures on the Moon 3 4 Ariel N. Deutscha, Gregory A. Neumannb, James W. Heada, Lionel Wilsona,c 5 6 aDepartment of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 7 02912, USA 8 bNASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 9 cLancaster Environment Centre, Lancaster University, Lancaster LA1 4YQ, UK 10 11 Corresponding author: Ariel N. Deutsch 12 Corresponding email: [email protected] 13 14 Date of re-submission: 5 April 2019 15 16 Re-submitted to: Icarus 17 Manuscript number: ICARUS_2018_549 18 19 Highlights: 20 • Four positive Bouguer gravity anomalies are analyzed on the Moon’s nearside. 21 • The amplitudes of the anomalies require a deep density contrast. 22 • One 190-km anomaly with crater-related topography is suggestive of mantle uplift. 23 • Marius Hills anomalies are consistent with intruded dike swarms. 24 • An anomaly south of Aristarchus has a crater rim and possibly magmatic intrusions. 25 26 Key words: 27 Moon; gravity; impact cratering; volcanism 1 28 Abstract 29 30 Four, quasi-circular, positive Bouguer gravity anomalies (PBGAs) that are similar in diameter 31 (~90–190 km) and gravitational amplitude (>140 mGal contrast) are identified within the central 32 Oceanus Procellarum region of the Moon. These spatially associated PBGAs are located south of 33 Aristarchus Plateau, north of Flamsteed crater, and two are within the Marius Hills volcanic 34 complex (north and south). Each is characterized by distinct surface geologic features suggestive 35 of ancient impact craters and/or volcanic/plutonic activity.
    [Show full text]
  • Development and Field Testing of Moonraker: a Four-Wheel Rover in Minimal Design
    Development and Field Testing of Moonraker: a Four-Wheel Rover in Minimal Design Kazuya Yoshida*, Nathan Britton*, John Walker* *Dept. of Aerospace Engineering, Tohoku University, Japan e-mail: yoshida, nathan, [email protected] Abstract A light-weight, four-wheel rover was developed as a research test platform for a low cost lunar exploration that could be conducted commercially near future. The name of the platform is MoonRaker, The purpose of the Moon- Raker development is investigate control techniques and physical performance for a lunar rover with minimal size, such as less than 10 kg. In this paper, the authors de- scribe the design, development and field testing results of the MoonRaker project. 1 Introduction In the Space Robotics Laboratory, Tohoku University, Japan, we developed a light-weight, four-wheel rover as Figure 1. An image of a lava tube skylight, a research test platform for a low cost lunar exploration Marius Hills Hole acquired by Lunar that could be conducted commercially near future. As a Reconnaissance Orbiter Narrow Angle case study, the requirements for the Google Lunar X-Prize Camera (M122584310LE). (GLXP) is considered. In the GLXP, more-than-500 m of traverse across the surface of the Moon and transmission of high quality video images to the Earth are set as the ing for water ice or Helium-3, But one of the most exciting minimum requirements [1]. targets for lunar exploration is potential caves on the sur- ffi As a technical partner of Team Hakuto, an o cial face of the moon. team of the GLXP challenge in Japan, the Space Robotics In recent years, researchers have speculated that un- Laboratory has been working on the development of mo- derground tubes or caves, similar to those found on Earth bile robots (rovers) for wheel-based traverse on the lunar in volcanic areas, may exist on the moon.
    [Show full text]
  • Detection of Buried Empty Lunar Lava Tubes Using Grail Gravity Data
    47th Lunar and Planetary Science Conference (2016) 1509.pdf DETECTION OF BURIED EMPTY LUNAR LAVA TUBES USING GRAIL GRAVITY DATA. R. Sood1, L. Chappaz1, H. J. Melosh1,2, K. C. Howell1, and C. Milbury2. 1School of Aeronautics and Astronautics, Purdue Uni- versity, West Lafayette, Indiana 47907, [email protected], 2Earth, Atmospheric and Planetary Science, Purdue University, West Lafayette, Indiana 47907. Introduction: As a part of NASA's Discovery Program, the Gravity Recovery and Interior Laboratory (GRAIL) spacecraft were launched in September 2011. The sister spacecraft, Ebb and Flow, mapped lunar gravity to an unprecedented precision [1]. High resolu- tion data is currently being utilized to gain a greater understanding of the Moon's interior. Through gravita- tional analysis of the Moon, subsurface features, such as potential buried empty lava tubes, have also been detected [2]. Lava tubes are of interest as possible hu- man habitation sites safe from cosmic radiation, mi- crometeorite impacts and temperature extremes. The existence of such natural caverns is now supported by Kaguya's discoveries [3] of deep pits that may poten- tially be openings to empty lava tubes. In the current investigation, GRAIL gravity data collected at different altitudes is utilized to detect the presence and extent of candidate empty lava tubes beneath the surface of the Figure 1: Free-air and Bouguer cross-correlation maps lunar maria. and free-air/Bouguer correlation along with regional Detection Strategy: Previous work done by Chap- topography in the vicinity of Marius Hills skylight. paz et al., (2014) makes use of two detection strategies based on gradiometry and cross-correlation to detect rrelation between free-air and Bouguer maps where a subsurface features.
    [Show full text]
  • Detection of Lunar Lava Tubes by Lunar Radar Sounder Onboard Selene (Kaguya)
    Lunar and Planetary Science XLVIII (2017) 1711.pdf DETECTION OF LUNAR LAVA TUBES BY LUNAR RADAR SOUNDER ONBOARD SELENE (KAGUYA). J. Haruyama1, T. Kaku1,2, R. Shinoda1,2, W. Miyake2, A. Kumamoto3, K. Ishiyama1, T. Nishibori1, K. Yamamoto1, K. Kurosawa4, A.I. Suzuki1, S.T. Crites1, T. Michikami5, Y. Yokota6, R. Sood7, H. J. Melosh7,8, L. Chappaz, K.C. Howell. 1Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan), 2Engineering Department, Tokai Universi- ty, 3Science Department, Tohoku University, 4Planetary Exploration Research Center, Chiba Institute of Technolo- gy, 5Faculty of Engineering, Kindai University, 6Faculty of Science, Kochi University, 7School of Aeronautics and Astronautics, Purdue University, 8Earth, Atmospheric and Planetary Science, Purdue University . E- Mail:haruyama.junichi_at_jaxa.jp (change “_at_” to @). Introduction: In 2009, three huge pits were dis- aperture radar (SAR) processing[9] with a synthetic covered on the Moon in image data acquired by the aperture of 5 km. The data set is available via the SELENE Terrain Camera. Their diameters and depths JAXA/SELENE (Kaguya) data archive.[10] are several tens of meters or more.[1-3] They are possi- Results: Figure 1 shows an A-scan diagram (pow- ble skylight holes opening on large subsurface caverns ers of received echo vs elevation of subsurface reflect- such as lava tubes, [1] by analogy with similar pits found ing the echo). The echo power was normalized to be on Mars.[4] This possibility was enhanced significantly zero dB for a standard surface echo level, and to be 0 by LRO oblique observations; large openings were km in elevation for the mean radius of 1737.4 km.
    [Show full text]
  • Technologies Enabling Exploration of Skylights, Lava Tubes and Caves
    Technologies Enabling Exploration of Skylights, Lava Tubes and Caves NASA Innovative Advanced Concepts (NIAC) Phase I FOR OFFICE OF THE CHIEF TECHNOLOGIST NATIONAL AERONAUTICS AND SPACE ADMINISTRATION GRANT NUMBER: NNX11AR42G AWARD DATE: SEPTEMBER 15, 2011 END DATE: SEPTEMBER 14, 2012 FINAL REPORT BY ASTROBOTIC TECHNOLOGY 4551 FORBES AVE #300 PITTSBURGH, PA 15213-3524 WILLIAM WHITTAKER, PRINCIPAL INVESTIGATOR Abstract Robotic exploration of skylights and caves can seek out life, investigate geology and origins, and open the subsurface of other worlds to humankind. However, exploration of these features is a daunting venture. Planetary voids present perilous terrain that requires innovative technologies for access, exploration, and modeling. This research developed technologies for venturing underground and conceived mission architectures for robotic expeditions that explore skylights, lava tubes and caves. The investigation identified effective designs for mobile robot architecture to explore sub-planetary features. Results provide insight into mission architectures, skylight reconnaissance and modeling, robot configuration and operations, and subsurface sensing and modeling. These are developed as key enablers for robotic missions to explore planetary caves. These results are compiled to generate “Spelunker”, a prototype mission concept to explore a lunar skylight and cave. The Spelunker mission specifies safe landing on the rim of a skylight, tethered descent of a power and communications hub, and autonomous cave exploration by hybrid
    [Show full text]
  • The Marius Hills Volcanic Complex: a Stratigraphic Study S
    Lunar and Planetary Science XXX 1180.pdf THE MARIUS HILLS VOLCANIC COMPLEX: A STRATIGRAPHIC STUDY S. K. Dunkin and D. J. Heather, Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK ([email protected] and [email protected]) Introduction: Marius Hills is a volcanic complex est FeO contents on the Moon. Volcanic features are covering an area of 35,000km2 in the south-central seen on both high- and low-Ti mare units with some, region of Oceanus Procellarum. It is host to a variety such as sinuous rilles, cutting through several flows of of volcanic landforms including sinuous rilles, low more than one unit. As noted by [5] and [7] there ap- domes, steep-sided domes and cones [1]. Previous pears to be no correlation between mare colour and work on this region include both photogeological volcanic features. Mare flows formed both before and studies [1,2,3] and, more recently, multispectral work after the sinuous rilles, as evidenced by the fact that from the Galileo [4] and Clementine missions [5,6,7]. some mare flows overlie part of Rille A (see below) Using the Clementine dataset, we have constructed a making it indistinguishable from the surrounding multispectral mosaic and FeO and TiO2 maps of the mare on the multispectral image. When seen on a Lu- Marius Hills region from 9-16N and 300-312E, in nar Orbiter photograph however, the presence of the order to determine the mare stratigraphy in the region. rille can still be seen at the point where the flow cov- Data Reduction: The Clementine data for this re- ers the rille, which suggests that the flow itself is thin gion was processed using the ISIS software and meth- relative to the depth of the rille.
    [Show full text]
  • Characterization of Previously Unidentified Lunar Pyroclastic Deposits Using Lunar Reconnaissance Orbiter Camera Data J
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117, E00H25, doi:10.1029/2011JE003893, 2012 Characterization of previously unidentified lunar pyroclastic deposits using Lunar Reconnaissance Orbiter Camera data J. Olaf Gustafson,1 J. F. Bell III,2,3 L. R. Gaddis,4 B. R. Hawke,5 and T. A. Giguere5,6 Received 1 July 2011; revised 31 March 2012; accepted 14 April 2012; published 8 June 2012. [1] We used a Lunar Reconnaissance Orbiter Camera (LROC) global monochrome Wide-angle Camera (WAC) mosaic to conduct a survey of the Moon to search for previously unidentified pyroclastic deposits. Promising locations were examined in detail using LROC multispectral WAC mosaics, high-resolution LROC Narrow Angle Camera (NAC) images, and Clementine multispectral (ultraviolet-visible or UVVIS) data. Out of 47 potential deposits chosen for closer examination, 12 were selected as probable newly identified pyroclastic deposits. Potential pyroclastic deposits were generally found in settings similar to previously identified deposits, including areas within or near mare deposits adjacent to highlands, within floor-fractured craters, and along fissures in mare deposits. However, a significant new finding is the discovery of localized pyroclastic deposits within floor-fractured craters Anderson E and F on the lunar farside, isolated from other known similar deposits. Our search confirms that most major regional and localized low-albedo pyroclastic deposits have been identified on the Moon down to 100 m/pix resolution, and that additional newly identified deposits are likely to be either isolated small deposits or additional portions of discontinuous, patchy deposits. Citation: Gustafson, J. O., J. F. Bell III, L. R. Gaddis, B.
    [Show full text]
  • Advances in Lunar Science from the Clementine Mission: a Decadal Perspective
    Advances in lunar science from the Clementine mission: A decadal perspective Mark Robinson∗ and Miriam Riner Center for Planetary Sciences, Northwestern University, 1850 Campus Drive, Evanston, IL 60208, USA. ∗e-mail: [email protected] The Clementine spacecraft orbited the Moon and acquired science data for 10 weeks in the Spring of 1994. During this time it collected global 11-band multispectral images and near global altimetry. Select areas of the Moon were imaged at 25 m/pixel in visible light and 60 m/pixel in thermal wavelengths. From these datasets a new paradigm for the evolution of the lunar crust emerged. The Moon is no longer viewed as a two-terrane planet, the Apollo samples were found not to represent the lunar crust as a whole, and the complexity of lunar crustal stratigraphy was further revealed. More than ten years later the Clementine datasets continue to significantly advance lunar science and will continue to do so as new measurements are returned from planned missions such as Chandrayaan, SELENE, and Lunar Reconnaissance Orbiter. This paper highlights the scientific research conducted over the last decade using Clementine data and summarizes the influence of Clementine on our understanding of the Moon. 1. Introduction Lunar compositional mapping by color differ- ence and spectroscopic methods has been known The Apollo lunar missions returned a wealth of since the 1960s. However, only the nearside of the data in the form of samples, in situ measure- Moon can be seen from Earth, individual Apollo ments, orbital remote sensing, and observations by sample stations are not resolvable from Earth, highly trained astronauts that served to charac- and telescopic spectral observations are limited to terize the geology of six locations in great detail.
    [Show full text]