Planetary Science : a Lunar Perspective
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Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
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. -
Craters in Shadow
Section 3: Craters in Shadow Kepler Copernicus Eratosthenes Seen it Clavius Seen it Section 3: Craters in Shadow Visibility: A pair of binoculars is the minimum requirement to see these features. When: Look for them when the terminator’s close by, typically a day before last quarter. Not all craters are best seen when the Sun is high in the lunar sky - in fact most aren’t! If craters aren’t par- ticularly bright or dark, they tend to disappear into the background when the Moon’s phase is close to full. These craters are best seen when the ‘terminator’ is nearby, or when the Sun is low in the lunar sky as seen from the crater. This causes oblique lighting to fall on the crater and create exaggerated shadows. Ultimately, this makes the crater look more dramatic and easier to see. We’ll use this effect for the next section on lunar mountains, but before we do, there are a couple of craters that we’d like to bring to your attention. Actually, the Moon is covered with a whole host of wonderful craters that look amazing when the lighting is oblique. During the summer and into the early autumn, it’s the later phases of the Moon are best positioned in the sky - the phases following full Moon. Unfortunately, this means viewing in the early hours but don’t worry as we’ve kept things simple. We just want to give you a taste of what a shadowed crater looks like for this marathon, so the going here is really pretty easy! First, locate the two craters Kepler and Copernicus which were marathon targets pointed out in Section 2. -
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. -
January 2019 Cardanus & Krafft
A PUBLICATION OF THE LUNAR SECTION OF THE A.L.P.O. EDITED BY: Wayne Bailey [email protected] 17 Autumn Lane, Sewell, NJ 08080 RECENT BACK ISSUES: http://moon.scopesandscapes.com/tlo_back.html FEATURE OF THE MONTH – JANUARY 2019 CARDANUS & KRAFFT Sketch and text by Robert H. Hays, Jr. - Worth, Illinois, USA September 24, 2018 04:40-05:04 UT, 15 cm refl, 170x, seeing 7/10, transparence 6/6. I drew these craters and vicinity on the night of Sept. 23/24, 2018. The moon was about 22 hours before full. This area is in far western Oceanus Procellarum, and was favorably placed for observation that night. Cardanus is the southern one of this pair and is of moderate depth. Krafft to the north is practically identical in size, and is perhaps slightly deeper. Neither crater has a central peak. Several small craters are near and within Krafft. The crater just outside the southeast rim of Krafft is Krafft E, and Krafft C is nearby within Krafft. The small pit to the west is Krafft K, and Krafft D is between Krafft and Cardanus. Krafft C, D and E are similar sized, but K is smaller than these. A triangular-shaped swelling protrudes from the north side of Krafft. The tiny pit, even smaller than Krafft K, east of Cardanus is Cardanus E. There is a dusky area along the southwest side of Cardanus. Two short dark strips in this area may be part of the broken ring Cardanus R as shown on the. Lunar Quadrant map. -
Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations*
Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations* F. Marchisa,g, J.E. Enriqueza, J. P. Emeryb, M. Muellerc, M. Baeka, J. Pollockd, M. Assafine, R. Vieira Martinsf, J. Berthierg, F. Vachierg, D. P. Cruikshankh, L. Limi, D. Reichartj, K. Ivarsenj, J. Haislipj, A. LaCluyzej a. Carl Sagan Center, SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, USA. b. Earth and Planetary Sciences, University of Tennessee 306 Earth and Planetary Sciences Building Knoxville, TN 37996-1410 c. SRON, Netherlands Institute for Space Research, Low Energy Astrophysics, Postbus 800, 9700 AV Groningen, Netherlands d. Appalachian State University, Department of Physics and Astronomy, 231 CAP Building, Boone, NC 28608, USA e. Observatorio do Valongo/UFRJ, Ladeira Pedro Antonio 43, Rio de Janeiro, Brazil f. Observatório Nacional/MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro - RJ, Brazil. g. Institut de mécanique céleste et de calcul des éphémérides, Observatoire de Paris, Avenue Denfert-Rochereau, 75014 Paris, France h. NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000, USA i. NASA/Goddard Space Flight Center, Greenbelt, MD 20771, United States j. Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27514, U.S.A * Based in part on observations collected at the European Southern Observatory, Chile Programs Numbers 70.C-0543 and ID 72.C-0753 Corresponding author: Franck Marchis Carl Sagan Center SETI Institute 189 Bernardo Ave. Mountain View CA 94043 USA [email protected] Abstract: We collected mid-IR spectra from 5.2 to 38 µm using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups. -
37845R CS3 Book Hatfield's Diaries.Indd
“H.M.A.S. PERTH” 1939 -1941 From the diaries of P.O. George Hatfield Published in Sydney Australia in 2009 Publishing layout and Cover Design by George Hatfield Jnr. Printed by Springwood Printing Co. Faulconbridge NSW 2776 1 2 Foreword Of all the ships that have flown the ensign of the Royal Australian Navy, there has never been one quite like the first HMAS Perth, a cruiser of the Second World War. In her short life of just less than three years as an Australian warship she sailed all the world’s great oceans, from the icy wastes of the North Atlantic to the steamy heat of the Indian Ocean and the far blue horizons of the Pacific. She survived a hurricane in the Caribbean and months of Italian and German bombing in the Mediterranean. One bomb hit her and nearly sank her. She fought the Italians at the Battle of Matapan in March, 1941, which was the last great fleet action of the British Royal Navy, and she was present in June that year off Syria when the three Australian services - Army, RAN and RAAF - fought together for the first time. Eventually, she was sunk in a heroic battle against an overwhelming Japanese force in the Java Sea off Indonesia in 1942. Fast and powerful and modern for her times, Perth was a light cruiser of some 7,000 tonnes, with a main armament of eight 6- inch guns, and a top speed of about 34 knots. She had a crew of about 650 men, give or take, most of them young men in their twenties. -
Phosphorus and Sulfur Cosmochemistry: Implications for the Origins of Life
Phosphorus and Sulfur Cosmochemistry: Implications for the Origins of Life Item Type text; Electronic Dissertation Authors Pasek, Matthew Adam Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 07/10/2021 06:16:37 Link to Item http://hdl.handle.net/10150/194288 PHOSPHORUS AND SULFUR COSMOCHEMISTRY: IMPLICATIONS FOR THE ORIGINS OF LIFE by Matthew Adam Pasek ________________________ A Dissertation Submitted to the Faculty of the DEPARTMENT OF PLANETARY SCIENCE In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College UNIVERSITY OF ARIZONA 2 0 0 6 2 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE As members of the Dissertation Committee, we certify that we have read the dissertation prepared by Matthew Adam Pasek entitled Phosphorus and Sulfur Cosmochemistry: Implications for the Origins of Life and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Philosophy _______________________________________________________________________ Date: 04/11/2006 Dante Lauretta _______________________________________________________________________ Date: 04/11/2006 Timothy Swindle _______________________________________________________________________ Date: 04/11/2006 -
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. -
Pete Aldridge Well, Good Afternoon, Ladies and Gentlemen, and Welcome to the Fifth and Final Public Hearing of the President’S Commission on Moon, Mars, and Beyond
The President’s Commission on Implementation of United States Space Exploration Policy PUBLIC HEARING Asia Society 725 Park Avenue New York, NY Monday, May 3, and Tuesday, May 4, 2004 Pete Aldridge Well, good afternoon, ladies and gentlemen, and welcome to the fifth and final public hearing of the President’s Commission on Moon, Mars, and Beyond. I think I can speak for everyone here when I say that the time period since this Commission was appointed and asked to produce a report has elapsed at the speed of light. At least it seems that way. Since February, we’ve heard testimonies from a broad range of space experts, the Mars rovers have won an expanded audience of space enthusiasts, and a renewed interest in space science has surfaced, calling for a new generation of space educators. In less than a month, we will present our findings to the White House. The Commission is here to explore ways to achieve the President’s vision of going back to the Moon and on to Mars and beyond. We have listened and talked to experts at four previous hearings—in Washington, D.C.; Dayton, Ohio; Atlanta, Georgia; and San Francisco, California—and talked among ourselves and we realize that this vision produces a focus not just for NASA but a focus that can revitalize US space capability and have a significant impact on our nation’s industrial base, and academia, and the quality of life for all Americans. As you can see from our agenda, we’re talking with those experts from many, many disciplines, including those outside the traditional aerospace arena. -
Impact Cratering in the Solar System
Impact Cratering in the Solar System Michelle Kirchoff Lunar and Planetary Institute University of Houston - Clear Lake Physics Seminar March 24, 2008 Outline What is an impact crater? Why should we care about impact craters? Inner Solar System Outer Solar System Conclusions Open Questions What is an impact crater? Basically a hole in the ground… Barringer Meteor Crater (Earth) Bessel Crater (Moon) Diameter = 1.2 km Diameter = 16 km Depth = 200 m Depth = 2 km www.lpi.usra.edu What creates an “impact” crater? •Galileo sees circular features on Moon & realizes they are depressions (1610) •In 1600-1800’s many think they are volcanic features: look similar to extinct volcanoes on Earth; some even claim to see volcanic eruptions; space is empty (meteorites not verified until 1819 by Chladni) •G.K. Gilbert (1893) first serious support for lunar craters from impacts (geology and experiments) •On Earth Barringer (Meteor) crater recognized as created by impact by Barringer (1906) •Opik (1916) - impacts are high velocity, thus create circular craters at most impact angles Melosh, 1989 …High-Velocity Impacts! www.lpl.arizona.edu/SIC/impact_cratering/Chicxulub/Animation.gif Physics of Impact Cratering Understand how stress (or shock) waves propagate through material in 3 stages: 1. Contact and Compression 2. Excavation 3. Modification www.psi.edu/explorecraters/background.htm Hugoniot Equations Derived by P.H. Hugoniot (1887) to describe shock fronts using conservation of mass, momentum and energy across the discontinuity. equation (U-up) = oU of state P-Po = oupU E-Eo = (P+Po)(Vo-V)/2 P - pressure U - shock velocity up - particle velocity E - specific internal energy V = 1/specific volume) Understanding Crater Formation laboratory large simulations explosives (1950’s) (1940’s) www.nasa.gov/centers/ames/ numerical simulations (1960’s) www.lanl.gov/ Crater Morphology • Simple • Complex • Central peak/pit • Peak ring www3.imperial.ac.