DOCSLIB.ORG

Lunar Orbiter V

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Lunar Orbiter V NASA CONTRACTOR NASA CR-1095 REPORT < V') < ::z: LUNAR ORBITER V Photographic Mission Summary Prepared by THE BOEING COMPANY Seattle, Wash. for Langley Research Center NATIONAL AERONAUTICS AND SPACE ADMINISTRATION • WASHINGTON, D. C. • JULY 1968 Hyginus Rille Photo taken by NASA-Boeing Lunar Orbiter V, August 14, 1967, 03:02:56 GMT from a distance of 65 miles. NASA CR-1095 LUNAR ORBITER V Photographic Mission Summary Distribution of this report is provided in the interest of information exchange. Responsibility for the contents resides in the author or organization that prepared it. Issued by Originator as Boeing Document 02-100755-1 (Vol. I) Prepared under Contract No. NAS 1-3800 by THE BOEING COMPANY . Seattle, Wash. for Langley Res~arch Center NATIONAL AERONAUTICS AND SPACE ADMINISTRATION For sale by the Clearinghouse for Federal Scientific and Technical Information Springfield, Virginia 22151- CFSTI price $3.00 Contents Page Lunar Orbiter V Photographic Mission Summary ..................................... 1 1.0 Introduction ...................................................................5 1.1 Program Description .......................................................5 1.2 Program Management ... ....... ... .. .. .. ... ...... .. .. ... ... .. ... ....... .. 5 1.3 Program Objectives ........................................................ 7 1.3.1 Mission V Objectives ..... ... .......................................... 7 1.4 Mission Design .. ....... .. ....... .. ........ ...... ........ .. .... ...... .. .. 8 1.5 Flight Vehicle Description ..... ... .. .. ........... .. .... .. ....... ..... ..... 13 2.0 Launch Preparation and Operations .. ... ... ... ........... ... .... .. ... .. .... .. 21 2.1 Launch Vehicle Preparation ...............................................21 2.2 Spacecraft Preparation .....................................................22 2.3 Launch Countdown .. .. ....... .. ..... .. .... ...... .... .. .... ... .. ........ 22 2.4 Launch Phase ................. .... ............. .... .... .............. .24 2.4.1 Flight Vehicle Performance .........................................24 2.5 Data Acquisition ..........................................................27 3.0 Mission Operations .. ......... .. ... ... .... ... ....... .. .... ... ... ... ..........31 3.1 Mission Profile .... .. ... .. .. .. ..................... .. .... .. .... .. ........31 3.2 Spacecraft Performance ....... .. .... ... .............. .. ..... .. ............33 3.2.1 Photo Subsystem Performance .... ....... .. ........ .. ...............34 3.2.2 Power Subsystem Performance .....................................37 3.2.3 Communications Subsystem Performance ....... ... .... ... ... .......39 3.2.4 Attitude Control Subsystem Performance ........................... .41 3.2.5 Velocity Control Subsystem Performance .......................... .44 3.2.6 Structures, Mechanisms, and Integration Elements Performance ...... .46 3.3 Operational Performance .............. ......... ... .. ... ... .. ........... .4 7 3.3.1 Spacecraft Control ............................................... .48 3.3.2 Flight Path Control ............................................... .49 3.4 Ground Systems Performance .............................................55 3.4.1 Space Flight Operations Facility ....................................55 3.4.2 Deep Space Stations . ... ......... ... ........... ... .... ......... .58 3.4.3 Ground Communications System .. ............ ... ... .... ... ... ......58 3.4.4 Photo Processing ...... .. ... .. .............. ... .. .... ......... .. ... .59 3.4.5 Langley Photo Data Assessment Facility .............................59 4.0 Mission Data ...............................................................63 4.1 Photographic Data . .. ......... ..... ... .. .... .......... ..... .... ... ......63 4.1.1 Mission Photography ................................................65 4.1.2 Photo Coverage .....................................................67 4.2 Environmental Data ..................................................... 128 4.2.1 Radiation Data ....... ... ......... ... ... ...... .. ............ .. .... 128 4.2.2 Micrometeoroid Data .............................................. 128 4.3 Tracking Data ................ ... ................ ..... ..... ......... ... 128 4.3.1 DSI F Tracking Data System ....................................... 128 4.3.2 DSN ............................................................. 130 4.4 Performance Telemetry ......................... .......... ..... ....... 130 5.0 Mission Evaluation ......................................................... 133 6.0 Program Summary .. ....... .. .............................................. 135 iii Figures Page Figure 1-1: Lunar Orbiter Project Organization .................................6 Figure 1-2: Photo Site Location - Nearside ....................................9 Figure 1-3: Planned Photo Period Sequence of Events ........................ 14 Figure 1-4: Exposure Sequences and Priority Readouts ........................ 15 Figure 1-5: Lunar Orbiter Spacecraft ......................................... 16 Figure 1-6: Lunar Orbiter Block Diagram .................................... 17 Figure 1-7: Photographic Data Acquisition, Reconstruction, and Assembly ..... 18 Figure 1-8: Launch Vehicle .................................................. 19 Figure 2-1: Launch Operations Flow Chart ....................................23 Figure 2-2: Master Countdown Time Sequence ...............................24 Figure 2-3: Ground Track for August 1, 1967 ..................................28 Figure 3-1: Lunar Orbiter V Flight Profile ............................... 32 Figure 3-2: Photo Subsystem ................................................. 35 Figure 3-3: Video Signal Waveform ..........................................36 Figure 3-4: Power Subsystem Block Diagram ...................................37 Figure 3-5: Communications Subsystem Block Diagram .......................39 Figure 3-6: Altitude Control Subsystem Functional Block Diagram ........... .42 Figure 3-7: Velocity and Reaction Control Subsystem ....................... .45 Figure 3-8: Earth Photo Spatial Geometry .....................................53 Figure 3-9: Perilune Altitude History ......................................... 56 Figure 3-10: Orbit Inclination History .........................................56 Figure 3-11: Argument of Perilune History ..................................... 57 Figure 3-12: Inertial Node Longitude History ..................................57 Figure 4-1: Altitude and Resolution Variation with Latitude ...................64 Figure 4-2: Pre-Exposed Reseau Mark Characteristics .........................65 Figure 4-3: Geometrical Parameters of Photography ...........................68 Figure 4-4: Selected Apollo Site Locations ....................................69 Figure 4-5: Scientifically Interesting Site Locations ..........................72 Figure 4-6: Scientifically Interesting "Landable" Site Locations ...............7 4 Figure 4-7: Farside Photo Coverage .......................................... 77 Figure 4-8 through 4-55: Selected Lunar Photographs (both wide angle and telephoto) ....80-127 Figure 4-56: Micrometeoroid Impact Geometry ................................ 129 Figure 6-l: Candidate Apollo Photo Site Locations ........................... 136 Figure 6-2: Lunar Farside Map (Polar Regions) ............................... 138 Figure 6-3: Lunar Farside Map (Midlatitudes) ................................ 139 iv Tables Page 1-1 Photo Site Coordinates ..................................................... 10 1-2 Launch Window Summary ................................................. 12 2-1 Launch Vehicle Preparation Summary ........................................21 2-2 Sequence of Significant Flight Events ......................................25 2-3 Electronic Tracking Coverage .............................................29 2-4 Telemetry Coverage ......................................................29 3-1 Trajectory Change Summary ..............................................34 3-2 L. 0. V Electrical Loads ..................................................38 3-3 Maneuver Summary ......................................................43 3-4 Gyro Drift Rates ......................................................... .44 3-5 Thruste Operation Summary ............................................. .44 3-6 Velocity Control Engine Performance ..................................... .45 3-7 Lunar Encounter Parameters ..............................................50 3-8 Summary of Encounter Parameters ........................................50 3-9 Initial Orbit Parameters ...................................................51 3-10 Intermediate-Ellipse Parameters ..........................................52 3-ll Final Transfer Results .....................................................54 3-12 Orbit 26 Parameters .......................................................54 3-13 Measured GRE Film Density .............................................59 4-1 Exposure Allocations .....................................................63 4-2 Supporting Data - Candidate Apollo Site ..................................70 4-3 Supporting Data- Scientifically Interesting "Landable" Sites ..............73 4-4 Supporting Data - Scientifically Interesting Sites .......................... 75 4-5 Supporting Data - Farside ............................................... 78 4-6 Radiation
Load more

Recommended publications
  • 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]
  • Radar Remote Sensing of Pyroclastic Deposits in the Southern Mare Serenitatis and Mare Vaporum Regions of the Moon Lynn M
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114, E11004, doi:10.1029/2009JE003406, 2009 Click Here for Full Article Radar remote sensing of pyroclastic deposits in the southern Mare Serenitatis and Mare Vaporum regions of the Moon Lynn M. Carter,1 Bruce A. Campbell,1 B. Ray Hawke,2 Donald B. Campbell,3 and Michael C. Nolan4 Received 21 April 2009; revised 12 July 2009; accepted 3 August 2009; published 5 November 2009. [1] We use polarimetric radar observations to study the distribution, depth, and embedded rock abundance of nearside lunar pyroclastic deposits. Radar images were obtained for Mare Vaporum and the southern half of Mare Serenitatis; the imaged areas contain the large Rima Bode, Mare Vaporum, Sulpicius Gallus, and Taurus-Littrow pyroclastic deposits. Potential pyroclastic deposits at Rima Hyginus crater, the Tacquet Formation, and a dome in Mare Vaporum are also included. Data were acquired at S band (12.6 cm wavelength) using Arecibo Observatory and the Green Bank Telescope in a bistatic configuration. The S band images have resolutions between 20 and 100 m/pixel. The pyroclastic deposits appear dark to the radar and have low circular polarization ratios at S band wavelengths because they are smooth, easily penetrable by radar waves, and generally contain few embedded blocks. Changes in circular polarization ratio (CPR) across some of the pyroclastic deposits show areas with increased rock abundance as well as deposits that are shallower. Radar backscatter and CPR maps are used to identify fine-grained mantling deposits in cases where optical and near-infrared data are ambiguous about the presence of pyroclastics.
    [Show full text]
  • Sky and Telescope
    SkyandTelescope.com The Lunar 100 By Charles A. Wood Just about every telescope user is familiar with French comet hunter Charles Messier's catalog of fuzzy objects. Messier's 18th-century listing of 109 galaxies, clusters, and nebulae contains some of the largest, brightest, and most visually interesting deep-sky treasures visible from the Northern Hemisphere. Little wonder that observing all the M objects is regarded as a virtual rite of passage for amateur astronomers. But the night sky offers an object that is larger, brighter, and more visually captivating than anything on Messier's list: the Moon. Yet many backyard astronomers never go beyond the astro-tourist stage to acquire the knowledge and understanding necessary to really appreciate what they're looking at, and how magnificent and amazing it truly is. Perhaps this is because after they identify a few of the Moon's most conspicuous features, many amateurs don't know where Many Lunar 100 selections are plainly visible in this image of the full Moon, while others require to look next. a more detailed view, different illumination, or favorable libration. North is up. S&T: Gary The Lunar 100 list is an attempt to provide Moon lovers with Seronik something akin to what deep-sky observers enjoy with the Messier catalog: a selection of telescopic sights to ignite interest and enhance understanding. Presented here is a selection of the Moon's 100 most interesting regions, craters, basins, mountains, rilles, and domes. I challenge observers to find and observe them all and, more important, to consider what each feature tells us about lunar and Earth history.
    [Show full text]
  • EXPLORING SUBSURFACE LUNAR VOIDS USING SURFACE GRAVIMETRY. Kieran A. Carroll, Da- Vid Hatch2, R. Ghent3, S. Stanley3, N. Urbancic3, Marie-Claude Williamson, W.B
    46th Lunar and Planetary Science Conference (2015) 1746.pdf EXPLORING SUBSURFACE LUNAR VOIDS USING SURFACE GRAVIMETRY. Kieran A. Carroll, Da- vid Hatch2, R. Ghent3, S. Stanley3, N. Urbancic3, Marie-Claude Williamson, W.B. Garry4, Manik Talwani5 1Gedex Inc., 407 Matheson Blvd. East, Mississauga, Ontario, Canada L4Z 2H2, [email protected], 2Gedex Inc., 3University of Toronto, 4NASA GSFC, 5Rice University. Introduction: Surface gravimetry is a standard been found to be linear but discontinuous…the space terrestrial geophysics exploration technique. As noth- between such features likely represents uncollapsed ing blocks gravity, this approach can detect subsurface tube.” structures with contrasting densities, both shallow and The structure of these voids is currently unknown, deep. Recently-collected high-resolution imagery of being unobservable via imagery from orbit. Lava tube the Moon has identified numerous pits, indicative of voids presumably might be like terrestrial lava tubes -- subsurface voids. Here we analyze the anomalous - long, linear or sinuous tunnels. In [5], Wagner et al. gravity signal expected at the Moon’s surface due to speculate that “a complex plumbing system may form both localized voids and more-extensive lava tubes, in some impact melt deposits,” and that “where multi- and find that the signal can be large enough to be ple pits were found in a single pond, the pits often oc- measured with Lunar-compatible gravimeters. A po- cur in one or more small regions (~2-5 km square) tential near-term Lunar surface survey of a mare pit within the melt deposit…occasionally, several pits crater in Lacus Mortis is discussed. occur within tens of meters of each other, indicating a possible subsurface connection.” Presumably some Lunar Lava Tubes and Other Subsurface other Lunar subsurface voids might instead be much Voids: Lava tubes can form when an exposed magma more compact, resulting from the draining of a single flow cools at its top surface, forming a solid “lid” over small melt pond.
    [Show full text]
  • 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.
    [Show full text]
  • Water on the Moon, III. Volatiles & Activity
    Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere).
    [Show full text]
  • Apollo Over the Moon: a View from Orbit (Nasa Sp-362)
    chl APOLLO OVER THE MOON: A VIEW FROM ORBIT (NASA SP-362) Chapter 1 - Introduction Harold Masursky, Farouk El-Baz, Frederick J. Doyle, and Leon J. Kosofsky [For a high resolution picture- click here] Objectives [1] Photography of the lunar surface was considered an important goal of the Apollo program by the National Aeronautics and Space Administration. The important objectives of Apollo photography were (1) to gather data pertaining to the topography and specific landmarks along the approach paths to the early Apollo landing sites; (2) to obtain high-resolution photographs of the landing sites and surrounding areas to plan lunar surface exploration, and to provide a basis for extrapolating the concentrated observations at the landing sites to nearby areas; and (3) to obtain photographs suitable for regional studies of the lunar geologic environment and the processes that act upon it. Through study of the photographs and all other arrays of information gathered by the Apollo and earlier lunar programs, we may develop an understanding of the evolution of the lunar crust. In this introductory chapter we describe how the Apollo photographic systems were selected and used; how the photographic mission plans were formulated and conducted; how part of the great mass of data is being analyzed and published; and, finally, we describe some of the scientific results. Historically most lunar atlases have used photointerpretive techniques to discuss the possible origins of the Moon's crust and its surface features. The ideas presented in this volume also rely on photointerpretation. However, many ideas are substantiated or expanded by information obtained from the huge arrays of supporting data gathered by Earth-based and orbital sensors, from experiments deployed on the lunar surface, and from studies made of the returned samples.
    [Show full text]
  • The Choice of the Location of the Lunar Base N93-17431
    155 PRECEDING PhGE ,,=,_,,c,;_''_'" t¢OT F|Lf_D THE CHOICE OF THE LOCATION OF THE LUNAR BASE N93-17431 V. V. Y__hevchenko P.. K _ AsO_nomtca/In./lute Moscow U_ Moscow 119899 USSR The development of modern methods of remote sensing of the lunar suuface and data from lunar studies by space vehicles make it possgale to assess scientifically the e:qOediowy of the locationof the lunar base in a definite region on the Moon. The prefimlnary choice of the site is important for tackling a range of problems assocfated with ensuring the activity of a manned lunar base and with fulfilh'ng the research program. Based on astronomical dat_ we suggest the Moon's western _, specifically the western part of Oceanus Proceliarurtg where natural scientifically interesting objects have been identifle_ as have surface rocks with enlaanced contents of ilmenite, a poss_le source of oxygen. A comprehensive et_tluation of the region shows timt, as far as natural features are concernetg it is a key one for solving the main problems of the Moon's orlgln and evolution. INTRODUCTION final period of shaping the lunar crust's upper horizons (this period coincided with the final equalization of the Moon's periods The main criteria for choosing a site for the first section of a of orbital revolution and axial rotation), the impact of terrestrial manned lunar base are (1)the most favorable conditions for gravitation on the internal structure of the Moon increased. transport operations, (2)the presence of natural objects of Between 4 and 3 b.y.
    [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]
  • Controls on Lunar Basaltic Volcanic Eruption Structure and Morphology: 2 Gas Release Patterns in Sequential Eruption Phases 3 L
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Lancaster E-Prints 1 Controls on Lunar Basaltic Volcanic Eruption Structure and Morphology: 2 Gas Release Patterns in Sequential Eruption Phases 3 L. Wilson1,2 and J. W. Head2 4 1Lancaster Environment Centre, Lancaster University, Lancaster LA1 4YQ, UK 5 2Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 6 02912 USA 7 8 Key Points: 9 Relationships between a diverse array of lunar mare effusive and explosive volcanic 10 deposits and landforms have previously been poorly understood. 11 Four stages in the generation, ascent and eruption of magma and gas release patterns are 12 identified and characterized. 13 Specific effusive, explosive volcanic deposits and landforms are linked to these four 14 stages in lunar mare basalt eruptions in a predictive and integrated manner. 15 16 Abstract 17 Assessment of mare basalt gas release patterns during individual eruptions provides the basis for 18 predicting the effect of vesiculation processes on the structure and morphology of associated 19 features. We subdivide typical lunar eruptions into four phases: Phase 1, dike penetrates to the 20 surface, transient gas release phase; Phase 2, dike base still rising, high flux hawaiian eruptive 21 phase; Phase 3, dike equilibration, lower flux hawaiian to strombolian transition phase; Phase 4, 22 dike closing, strombolian vesicular flow phase. We show how these four phases of mare basalt 23 volatile release, together with total dike volumes, initial magma volatile content, vent 24 configuration and magma discharge rate, can help relate the wide range of apparently disparate 25 lunar volcanic features (pyroclastic mantles, small shield volcanoes, compound flow fields, 26 sinuous rilles, long lava flows, pyroclastic cones, summit pit craters, irregular mare patches 27 (IMPs) and ring moat dome structures (RMDSs)) to a common set of eruption processes.
    [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]
  • Thorium Content of Mare Basalts of the Western Procellarum Region
    1 1 THORIUM CONTENT OF MARE BASALTS OF THE WESTERN PROCELLARUM REGION. B. L. Jolliff , J. J. Gillis , D. J. Lawrence2, and S. Maurice3, 1Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA; 2Los Alamos National Laboratory, MS-D466, Los Alamos NM 87545, USA; 3Observatoire Midi Pyrénées, 14 avenue Edouard Belin, 31400 Toulouse, France. ([email protected]) Introduction: Thorium data from the Lunar Pros- common 2° grid for FeO-TiO2-Th correlations, and for pector gamma-ray spectrometer (LPGRS) reveal a Th- a subset of areas, Th is resampled to 0.5 degree resolu- rich province in the Procellarum-Imbrium region that tion. Clementine data are from the 1999 USGS release has been called the Procellarum KREEP Terrane (PKT) [12] and we used the method described by [10] to [1-3]. Although it was known from Apollo gamma-ray calculate FeO and TiO2 profiles. results that a Th-rich province occurs in this region, In this abstract, we focus on a region from 6°S to LPGRS data showed clearly the extent of Th enrich- 26°N latitude and from 23°W to 63°W longitude. This ment. An unanticipated result was that within the PKT, area includes the crater Kepler on the eastern side and most areas, not just those exposing Imbrium ejecta such extends westward across Imbrian and Eratosthenian as the Fra Mauro and Alpes Formations, have elevated flows, including the region around Marius and Reiner Th concentrations relative to nearly all other regions of (Fig. 1). Basalts in this region include some that have the Moon’s surface.
    [Show full text]