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Geoscience and a Lunar Base
" t N_iSA Conference Pubhcatmn 3070 " i J Geoscience and a Lunar Base A Comprehensive Plan for Lunar Explora, tion unclas HI/VI 02907_4 at ,unar | !' / | .... ._-.;} / [ | -- --_,,,_-_ |,, |, • • |,_nrrr|l , .l -- - -- - ....... = F _: .......... s_ dd]T_- ! JL --_ - - _ '- "_r: °-__.......... / _r NASA Conference Publication 3070 Geoscience and a Lunar Base A Comprehensive Plan for Lunar Exploration Edited by G. Jeffrey Taylor Institute of Meteoritics University of New Mexico Albuquerque, New Mexico Paul D. Spudis U.S. Geological Survey Branch of Astrogeology Flagstaff, Arizona Proceedings of a workshop sponsored by the National Aeronautics and Space Administration, Washington, D.C., and held at the Lunar and Planetary Institute Houston, Texas August 25-26, 1988 IW_A National Aeronautics and Space Administration Office of Management Scientific and Technical Information Division 1990 PREFACE This report was produced at the request of Dr. Michael B. Duke, Director of the Solar System Exploration Division of the NASA Johnson Space Center. At a meeting of the Lunar and Planetary Sample Team (LAPST), Dr. Duke (at the time also Science Director of the Office of Exploration, NASA Headquarters) suggested that future lunar geoscience activities had not been planned systematically and that geoscience goals for the lunar base program were not articulated well. LAPST is a panel that advises NASA on lunar sample allocations and also serves as an advocate for lunar science within the planetary science community. LAPST took it upon itself to organize some formal geoscience planning for a lunar base by creating a document that outlines the types of missions and activities that are needed to understand the Moon and its geologic history. -
No. 40. the System of Lunar Craters, Quadrant Ii Alice P
NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates. -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
Planetary Surfaces
Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I]. -
Science Concept 5: Lunar Volcanism Provides a Window Into the Thermal and Compositional Evolution of the Moon
Science Concept 5: Lunar Volcanism Provides a Window into the Thermal and Compositional Evolution of the Moon Science Concept 5: Lunar volcanism provides a window into the thermal and compositional evolution of the Moon Science Goals: a. Determine the origin and variability of lunar basalts. b. Determine the age of the youngest and oldest mare basalts. c. Determine the compositional range and extent of lunar pyroclastic deposits. d. Determine the flux of lunar volcanism and its evolution through space and time. INTRODUCTION Features of Lunar Volcanism The most prominent volcanic features on the lunar surface are the low albedo mare regions, which cover approximately 17% of the lunar surface (Fig. 5.1). Mare regions are generally considered to be made up of flood basalts, which are the product of highly voluminous basaltic volcanism. On the Moon, such flood basalts typically fill topographically-low impact basins up to 2000 m below the global mean elevation (Wilhelms, 1987). The mare regions are asymmetrically distributed on the lunar surface and cover about 33% of the nearside and only ~3% of the far-side (Wilhelms, 1987). Other volcanic surface features include pyroclastic deposits, domes, and rilles. These features occur on a much smaller scale than the mare flood basalts, but are no less important in understanding lunar volcanism and the internal evolution of the Moon. Table 5.1 outlines different types of volcanic features and their interpreted formational processes. TABLE 5.1 Lunar Volcanic Features Volcanic Feature Interpreted Process -
Relative Ages
CONTENTS Page Introduction ...................................................... 123 Stratigraphic nomenclature ........................................ 123 Superpositions ................................................... 125 Mare-crater relations .......................................... 125 Crater-crater relations .......................................... 127 Basin-crater relations .......................................... 127 Mapping conventions .......................................... 127 Crater dating .................................................... 129 General principles ............................................. 129 Size-frequency relations ........................................ 129 Morphology of large craters .................................... 129 Morphology of small craters, by Newell J. Fask .................. 131 D, method .................................................... 133 Summary ........................................................ 133 table 7.1). The first three of these sequences, which are older than INTRODUCTION the visible mare materials, are also dominated internally by the The goals of both terrestrial and lunar stratigraphy are to inte- deposits of basins. The fourth (youngest) sequence consists of mare grate geologic units into a stratigraphic column applicable over the and crater materials. This chapter explains the general methods of whole planet and to calibrate this column with absolute ages. The stratigraphic analysis that are employed in the next six chapters first step in reconstructing -
Compositional and Mineralogical Characteristics of Archimedes Crater Region Using Chandrayaan – 1 M3 Data
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1040.pdf COMPOSITIONAL AND MINERALOGICAL CHARACTERISTICS OF ARCHIMEDES CRATER REGION USING CHANDRAYAAN – 1 M3 DATA. P. R. Kumaresan1 and J. Saravanavel2, 1Research Scholar, 2Assistant Professor, Department of Remote Sensing, Bharathidasan University, Tiruchirappalli-23, Tamil Nadu, India, email: [email protected], [email protected] Introduction: The Earth’s natural satellite the tometry corrected reflectance data captured during the moon is nearest celestial body appears brightest object OP1B optical period. in our night sky. Moon surfaces are composed of dark and light areas. The dark areas are called Maria which is made up of basaltic terrain and light areas are high- lands mostly made up of Anorthositic rocks. The moon surface is littered with craters, which are formed when meteors hit its surface. To understand the evolution, geological process of the moon it is important to study the surface composition and minerals present in crustal surface. In this regard, in our study, we have attempted to map the minerals and surface composition of Archi- medes crater region. Study area: Archimedes crater is a large impact crater located on the eastern edges of the Mare Imbri- um of near side moon (29.7° N, 4.0° W). The diameter of the crater is 83 km with smooth floor flooded (1) with mare basalt and lack of a central peak. The rim (2) has a significant outer rampart brightened with ejecta (3) and the some portion of a terraced inner wall. Ar- chimedes Crater is named for the Greek mathematician Archimedes, who made many mathematical discoveries in the 200 B.C [1, 2]. -
Tectonic Evolution of Northwestern Imbrium of the Moon That Lasted In
Daket et al. Earth, Planets and Space (2016) 68:157 DOI 10.1186/s40623-016-0531-0 FULL PAPER Open Access Tectonic evolution of northwestern Imbrium of the Moon that lasted in the Copernican Period Yuko Daket1* , Atsushi Yamaji1, Katsushi Sato1, Junichi Haruyama2, Tomokatsu Morota3, Makiko Ohtake2 and Tsuneo Matsunaga4 Abstract The formation ages of tectonic structures and their spatial distributions were studied in the northwestern Imbrium and Sinus Iridum regions using images obtained by Terrain Camera and Multiband Imager on board the SELENE spacecraft and the images obtained by Narrow Angle Camera on board LRO. The formation ages of mare ridges are constrained by the depositional ages of mare basalts, which are either deformed or dammed by the ridges. For this purpose, we defined stratigraphic units and determined their depositional ages by crater counting. The degradation levels of craters dislocated by tectonic structures were also used to determine the youngest limits of the ages of the tectonic activities. As a result, it was found that the contractions to form mare ridges lasted long after the deposition of the majority of the mare basalts. There are mare ridges that were tectonically active even in the Copernican Period. Those young structures are inconsistent with the mascon tectonics hypothesis, which attributes tectonic deforma- tions to the subsidence of voluminous basaltic fills. The global cooling or the cooling of the Procellarum KREEP Ter- rane region seems to be responsible for them. In addition, we found a graben that was active after the Eratosthenian Period. It suggests that the global or regional cooling has a stress level low enough to allow the local extensional tectonics. -
On the Moon with Apollo 16. a Guidebook to the Descartes Region. INSTITUTION National Aeronautics and Space Administration, Washington, D.C
DOCUMENT RESUME ED 062 148 SE 013 594 AUTHOR Simmons, Gene TITLE On the Moon with Apollo 16. A Guidebook to the Descartes Region. INSTITUTION National Aeronautics and Space Administration, Washington, D.C. REPORT NO NASA-EP-95 PUB DATE Apr 72 NOTE 92p. AVAILABLE FROM Superintendent of Documents, Government Printing Office, Washington, D. C. 20402 (Stock Number 3300-0421, $1.00) EDRS PRICE MF-$0.65 HC-$3.29 DESCRIPTORS *Aerospace Technology; Astronomy; *Lunar Research; Resource Materials; Scientific Research; *Space Sciences IDENTIFIERS NASA ABSTRACT The Apollo 16 guidebook describes and illustrates (with artist concepts) the physical appearance of the lunar region visited. Maps show the planned traverses (trips on the lunar surface via Lunar Rover); the plans for scientific experiments are described in depth; and timelines for all activities are included. A section on uThe Crewn is illustrated with photos showing training and preparatory activities. (Aathor/PR) ON THE MOON WITH APOLLO 16 A Guidebook to the Descartes Region U.S. DEPARTMENT OF HEALTH. EDUCATION & WELFARE OFFICE OF EDUCATION THIS DOCUMENT HAS BEEN REPRO- DUCED EXACTLY AS RECEIVED FROM THE PERSON OR ORGANIZATION ORIG- grIl INATING IT POINTS OF VIEW OR OPIN- IONS STATED DO NOT NECESSARILY REPRESENT OFFICIAL OFFICE OF EDU- CATION POSITION on POLICY. JAI -0110 44 . UP. 16/11.4LI NATIONAL AERONAUTICS AND SPACE ADMINISTRATION April 1972 EP-95 kr) ON THE MOON WITH APOLLO 16 A Guidebook to the Descartes Region by Gene Simmons A * 40. 7 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION April 1972 2 Gene Simmons was Chief Scientist of the Manned Spacecraft Center in Houston for two years and isnow Professor of Geophysics at the Mas- sachusetts Institute of Technology. -
TARGET DATE Latitude Longitude ARCHIMEDES N. WALL 10/23
TARGET DATE Latitude Longitude ARCHIMEDES N. WALL 10/23/1983 TYCHO SW WALL 10/23/1983 GRUIT CRATER NEAR DOMES 10/23/1983 BULLIALDUS CENTRAL PEAK 10/26/1983 CRATER NR. EICHSTADT 10/27/1983 ARISTARCHUS S. WALL 1 10/27/1983 HERODOTUS X 8/3/1980 23.2 ‐49.7 REINER K 8/3/1980 8.1 ‐53.9 REINER GAMMA TAIL 2 8/3/1980 7.8 ‐57.7 REINER GAMMA 8/3/1980 7.4 ‐58.8 BYRGIUS 7/25/1983 ‐24.7 ‐65.3 INGHIRAMI W BOWL 8/17/1981 ‐44.4 ‐67.3 TYCHO FLOOR 7/13/1981 TYCHO WALL 7/13/1981 TYCHO HALO 7/13/1981 COPERNICUS EJECTA 2 7/15/1981 COPERNICUS EJECTA 4 7/15/1981 APOLLO 14 8/2/1980 APOLLO 14 WEST CRATER 8/2/1980 PLATO RADAR 1 9/5/1982 ARISTARCHUS PLATEAU PEAK 1 9/6/1982 COBRA HEAD 10/22/1983 NE AGRICOLA MTS 2 10/22/1983 TYCHO SW FLOOR 10/23/1983 ARCHIMEDES N. WALL 1 10/23/1983 TYCHO SW WALL 10/23/1983 GRUIT CRATER NEAR DOMES 10/23/1983 BULLIALDUS CENTRAL PEAK 10/26/1983 CRATER NR. EICHSTADT 10/27/1983 ARISTARCHUS S. WALL 1 10/27/1983 ARISTARCHUS S. WALL 2 10/27/1983 Bright Spot, NR. S. RIM CREST 10/27/1983 ARISTARCHUS N. WALL 10/27/1983 S.LACUS AUTUMNI 10/28/1983 S. HIGHLAND REGION A 11/5/1976 COPERNICUS PEAK 1 11/24/1980 COPERNICUS WALL 1 11/24/1980 MS 2 7/13/1981 SOUTH SWIRL 8/3/1980 MARIUS HILLS 11/24/1980 ARCHIMEDES N.WALL#1 /SUN 10/23/83 AP.2 2.5 2.0 (j.) () c .....0 () (j.) ..... -
Volcanism on Mercury
SPECIALSECTION theLRMarealsoseenintheMASCSdata(30). References and Notes 22. P. G. Lucey, D. T. Blewett, B. L. Jolliff, J. Geophys. Res. From these observations and previous work 1. S. E. Hawkins III et al., Space Sci. Rev. 131, 247 (2007). 105, 20297 (2000). 2–7 10 18 21 ’ 2. T. B. McCord, J. B. Adams, Icarus 17, 585 (1972). 23. G. Heiken, D. T. Vaniman, B. M. French, Lunar ( , , , ), we propose that Mercury scrust 3. B. Hapke, G. E. Danielson Jr., K. Klaasen, L. Wilson, Sourcebook: A User's Guide to the Moon (Cambridge is composed of iron-poor calcium-magnesium sili- J. Geophys. Res. 80, 2431 (1975). Univ. Press, New York, 1991). cates (e.g., plagioclase, enstatite, pigeonite, and diop- 4. J. Warell, Icarus 161, 199 (2003). 24. S. K. Noble, C. M. Pieters, Sol. Syst. Res. 37, 31 (2003). side) with a detectable component of spectrally 5. F. Vilas, in Mercury,F.Vilas,C.R.Chapman,M.S.Mathews, 25. M. J. Cintala, J. Geophys. Res. 97, 947 (1992). – Meteorit. Planet. neutral opaque minerals. Ilmenite (FeTiO )isthe Eds. (Univ. of Arizona Press, Tucson, 1988), pp. 59 76. 26. D. T. Blewett, B. R. Hawke, P. G. Lucey, 3 6. A. L. Sprague, T. L. Roush, Icarus 133, 174 (1998). Sci. 37, 1245 (2002). most likely candidate based on lunar analogy and 7. J. Warell, D. T. Blewett, Icarus 168, 257 (2004). 27. B. R. Hawke, P. G. Lucey, J. F. Bell, R. Jaumann, G. Neukum, cosmochemical abundance considerations. This 8. B. Hapke, J. Geophys. Res. 106, 10039 (2001). Lunar Planet. -
Tossup Roentgen, Archimedes, Gauss, Balboa an D~¥As.:.? Da
Tossup , Roentgen, Archimedes, Gauss, Balboa an_d ~¥as.:.? Da Gama all have one bigger than Einstein's. Rutherford's is inside of..G!avius'. ' ~e three largest are Hertzsprung, Korolev and Apollo. For 10 points );IlUlt are t!1e~ objects, seven of which will be named for the astronauts who ~e..s-p~ttle disaster. / . Lunar Craters (' ,/ J- This Athenjan wa~ an admirer of Socrates ~ndji . him' such works as the Symposium and the Apo!?gy of Socrates. ~ - - st known wever, as an historian, the author of the Hellemca and the AnaEiastS, an a t of a mercenary expedition into Asia Minor. For 10 points, name ntury B.C. author. Xenophon ,. .. .. "The seizure of $3~&;gWo Y Hills," "Savage Lu~y ... 'Teeth Like Baseballs, Eyes Like J llied ire, '" and "A Terrible Experience with Extremely Dangerous Drugs." These e apters from, for 10 points, .what book? Fear and Loathing in Las Vegas (by Hunter S. Thompson) .' Lazlo Toth attacked her with a h~e, screaming "I Jesus Christ". He severed her left arm, smas~er nose-and lsfigured her I eye. That was in 1972, and today she and her ~n~i~ ·- behlnd i ss wall in J) Peter's Basilica the scars barely visible. For 10 y.Qin(s, "Yho are .... y, re ? ' The Pieul . L/ Accept: C~st and the Virgin Mary In 1649She invited Rene Descartes to her court to teach her philosophy. She had her lessons at 5 in the morning; Des.cartes, more used to rising at noon, caught a c . d died. Fo t's: who was this Swedish queen, \ the daughter of Gustavus Christina \, \ \ / Tossup Its biological name Ailuropod I 'l- " --~ .