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RESALE Numberor Stating You Are a Retailor In
TucsonAuction08.html 9th Annual Tucson Meteorite Auction ----------------------------- Tucson Meteorite Auction 2008 Saturday, February 9th, 2008 Bidding starts 7:30PM Sharp Viewing & Socializing begins 5:30PM Food and Drink available http://www.michaelbloodmeteorites.com/TucsonAuction08.html (1 z 36) [2008-05-28 18:09:44] TucsonAuction08.html (Please drink only with a designated driver) ----------------------- While in Tucson I will have a cell phone: (619) 204-4138 (Feb2-Feb10) NEW LOCATION VFW Hall (Post # 549) 1884 So. Craycroft, Tucson, AZ 85711 (see directions below) NOTE: Click HERE for printer friendly copy of this catalog (Click on any photo to see a greatly enlarged image) 1 AH 1 Claxton L6, GeorgiaDecember 10 th , 1984 - Hit A Mailbox! .992g Rim Crusted Part Slice (21mm X 20mm X 2mm) No Minimum 2 AH 2 Dhofar 908 Lunar Meteorite - Rosetta - 1.242g Full Slice (24mm X 16mm X 2mm) No Minaimum - (est: $2.5K min) 3 AH 3 NWA 2999 Angrite Famous Paper "The Case For Samples From Mercury" 3.216g FC End Piece (18mm X 15mm X 7mm) No Minimum http://www.michaelbloodmeteorites.com/TucsonAuction08.html (2 z 36) [2008-05-28 18:09:44] TucsonAuction08.html 4 AH 4 NWA 4473 Polymict Diogenite 13g Full Slice(70mm X 13mm X ~2.5mm) No Minimum 5 AH 5 NWA 4880 (Shergottite) .540g 70% F Crusted Whole Stone (11mm X 9mm X 5mm) No Minimum 6 AH 6 NWA 4880 (Shergottite) 32.3g 92% FC Oriented Main Mass (35mm X 32mm X 32mm) Minimum Bid: $12,900.00 (Less Than $400/g) 7 AH 7 Oued el Hadjar (LL6) Fall March 1986 - "The Wedding Stone" 6.322 g (41mm X 30m X 3mm) The stone was broken into many pieces, then sacrificed on an alter during a wedding ceremony. -
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. -
Zinc and Copper Isotopic Fractionation During Planetary Differentiation Heng Chen Washington University in St
Washington University in St. Louis Washington University Open Scholarship Arts & Sciences Electronic Theses and Dissertations Arts & Sciences Winter 12-15-2014 Zinc and Copper Isotopic Fractionation during Planetary Differentiation Heng Chen Washington University in St. Louis Follow this and additional works at: https://openscholarship.wustl.edu/art_sci_etds Part of the Earth Sciences Commons Recommended Citation Chen, Heng, "Zinc and Copper Isotopic Fractionation during Planetary Differentiation" (2014). Arts & Sciences Electronic Theses and Dissertations. 360. https://openscholarship.wustl.edu/art_sci_etds/360 This Dissertation is brought to you for free and open access by the Arts & Sciences at Washington University Open Scholarship. It has been accepted for inclusion in Arts & Sciences Electronic Theses and Dissertations by an authorized administrator of Washington University Open Scholarship. For more information, please contact [email protected]. WASHINGTON UNIVERSITY IN ST. LOUIS Department of Earth and Planetary Sciences Dissertation Examination Committee: Bradley L. Jolliff, Chair Jeffrey G. Catalano Bruce Fegley, Jr. Michael J. Krawczynski Frédéric Moynier Zinc and Copper Isotopic Fractionation during Planetary Differentiation by Heng Chen A dissertation presented to the Graduate School of Arts & Sciences of Washington University in partial fulfillment of the requirements for the degree of Doctor of Philosophy December 2014 St. Louis, Missouri Copyright © 2014, Heng Chen All rights reserved. Table of Contents LIST OF FIGURES -
October 2006
OCTOBER 2 0 0 6 �������������� http://www.universetoday.com �������������� TAMMY PLOTNER WITH JEFF BARBOUR 283 SUNDAY, OCTOBER 1 In 1897, the world’s largest refractor (40”) debuted at the University of Chica- go’s Yerkes Observatory. Also today in 1958, NASA was established by an act of Congress. More? In 1962, the 300-foot radio telescope of the National Ra- dio Astronomy Observatory (NRAO) went live at Green Bank, West Virginia. It held place as the world’s second largest radio scope until it collapsed in 1988. Tonight let’s visit with an old lunar favorite. Easily seen in binoculars, the hexagonal walled plain of Albategnius ap- pears near the terminator about one-third the way north of the south limb. Look north of Albategnius for even larger and more ancient Hipparchus giving an almost “figure 8” view in binoculars. Between Hipparchus and Albategnius to the east are mid-sized craters Halley and Hind. Note the curious ALBATEGNIUS AND HIPPARCHUS ON THE relationship between impact crater Klein on Albategnius’ southwestern wall and TERMINATOR CREDIT: ROGER WARNER that of crater Horrocks on the northeastern wall of Hipparchus. Now let’s power up and “crater hop”... Just northwest of Hipparchus’ wall are the beginnings of the Sinus Medii area. Look for the deep imprint of Seeliger - named for a Dutch astronomer. Due north of Hipparchus is Rhaeticus, and here’s where things really get interesting. If the terminator has progressed far enough, you might spot tiny Blagg and Bruce to its west, the rough location of the Surveyor 4 and Surveyor 6 landing area. -
Glossary of Lunar Terminology
Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites. -
1962-11 Millman
MINUTES SPECIAL COUNCIL MEETING OF THE METEORITICAL SOCIETY held at Los Angeles, Calif., Sat., 17 Nov. 1962 PRESENT: President Peter M. Millman, Past-President John A. Russell, Editor Dorrit Hoffleit, Councilor C. H. Cleminshaw, and Secretary Gerald L. Rowland. Since Peter Millman and Dorrit Hoffleit were both in Los Angeles at the same time, and since it was possible to get a quorum of the Council together, President Millman called a Special meeting of the Council for Sat., 17 Nov. 1962. The last Council minutes (of 4 Sept., 1962) were read in order that those present might know the business that was transacted at Socorro, New Mexico. After some discussion, it was moved, seconded, and approved that arrangements be made for the transfer of a suitable number (approximately 40) of the 4 issues of Vol. I of Meteoritics from Springer Transfer Co. in Albuquerque, N. M., to John Russell at U.S.C. The Council approved the expenditure of whatever funds are necessary for this operation. John Russell reported that the Leonard Memorial Medal, which was displayed at the Socorro meeting, was unsatisfactory and that it is being re-done by the Southern California Trophy Co. The Council was reminded that the fund established for the Leonard Memorial Medal is still open for contributions. The cost of engraving and striking each individual medal to be presented will call for a nominal expenditure from time to time. The Council next suggested the following chairmen (subject to the individual's acceptance) for the standing committees of the Society: Eugene Shoemaker (Membership and Fellowship); Oscar Monnig (Finance and Endowment); Editor Dorrit Hoffleit (Publications). -
IWLOP Logbook
Isabel Williamson Lunar Observing Logbook The certificate applicant must use this logbook (or an equivant means) to qualify. Enter the date, time, and other details for each observation as indicated. The R (required) objectives are mandatory; the C (challenge) objectives are optional. Sketch drawings are also optional, but encouraged. Use the small template provided, or the larger one found on p. 84 of this logbook. PART 1 – Introducing the Moon A – Lunar Phases and Orbital Motion R 1 – Enter in the notes section the date and time for each phase observed. R 2 – Date _________________ Time__________________ R 3 – Date _________________ Time__________________ Date _________________ Time__________________ Notes _________________________________________________ _________________________________________________ _________________________________________________ _________________________________________________ B – Major Basins (Maria) & Pickering Unaided Eye Scale R 1 – Date __________________ Time__________________ C 1 – Date __________________ Time__________________ C 2 – Date __________________ Time__________________ Notes (see p. 81 of this logbook for optional Pickering Unaided Eye Scale) __________________________________________________ __________________________________________________ __________________________________________________ __________________________________________________ C – Ray System Extent R 1 – Date ___________________ Time_________________ C 1 – Date ___________________ Time_________________ Notes (see p. 82 of this -
Mini-Rf Radar Observations of Polar Craters: Are They Rough, Smooth, Or Icy?
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 2861.pdf MINI-RF RADAR OBSERVATIONS OF POLAR CRATERS: ARE THEY ROUGH, SMOOTH, OR ICY?. G. W. Patterson1, L. M. Jozwiak1, R. Kirk2, T. L. Becker2, R. Perkins3, L. M. Carter4, A. M. Stickle1, J. T. S. Cahill1, B. J. Thomson5, C. D. Neish6 and the Mini-RF team 1Planetary Exploration Group, Johns Hopkins University Applied Physics Laboratory, Laurel, MD ([email protected]), 2U.S. Geological Survey, Astrogeology Science Center, Flagstaff AZ, 3Department of Earth and Environmental Sciences, Wesleyan University, Middletown, CT, 4Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 5 Dept. of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, 6University of Western Ontario, London, ON, Canada. Introduction: The possibility that water ice could antenna operated as a transmitter and receiver. In this be present in lunar polar craters has long been operational mode, it transmitted a left-circular polarized postulated [e.g., 1,2]. More recently, measurements signal and received orthogonal linear polarizations [14]. from instruments on a number of spacecraft have all In December of 2010 the transmitter experienced a pointed to the presence of water at the lunar poles [e.g., malfunction and ceased to operate, precluding further 3-7]. The Lunar Crater Observation and Sensing monostatic data collection. Prior to this malfunction, Satellite (LCROSS) impact into a permanently Mini-RF was able to collect S-band data that covered > shadowed portion of Cabeus crater (84.9°S, 35.5°W; 98 66% of the lunar surface and > 95% of the lunar poles. -
The Oscar E. Monnig Meteorite Collection and Museum. Rg
41st Lunar and Planetary Science Conference (2010) 1162.pdf THE OSCAR E. MONNIG METEORITE COLLECTION AND MUSEUM. R. G. Mayne1 and T. Moss1 De- partment of Geology, TCU Box 298830, Texas Christian University, Fort Worth, TX 76109 ([email protected]) The Man Behind the Meteorites [1]: Oscar not knowing the full extent of what was to come. In Monnig was born in Fort Worth, Texas in 1902, and he the years that followed a number of meteorites were lived there till his death in 1999. He was a business- transferred to TCU, but it was not until his death in man and he started work for his family’s dry goods 1999 that the full generosity of Oscar’s offer came to company after earning his law degree from the Univer- light. TCU not only inherited all of Oscar’s meteorite sity of Texas in 1925 and was the CEO of the company collection, but also a large amount of his estate for when it was sold in 1982. However, Oscar’s passion “education, care, and maintenance of the meteorite was for meteorites, he was an avid collector. He even collection.” gave self-printed brochures to his traveling salesmen to The Monnig Meteorite Collection at TCU: The distribute that described how to identify meteorites and collection donated by Oscar Monnig was one of the offered to purchase any that were found. finest private collections of its day, and it is now one In 1960 Oscar Monnig introduced himself to a new of the finest University-based collections in the world, hire in the TCU Geology department, Dr. -
GRAIL Gravity Observations of the Transition from Complex Crater to Peak-Ring Basin on the Moon: Implications for Crustal Structure and Impact Basin Formation
Icarus 292 (2017) 54–73 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus GRAIL gravity observations of the transition from complex crater to peak-ring basin on the Moon: Implications for crustal structure and impact basin formation ∗ David M.H. Baker a,b, , James W. Head a, Roger J. Phillips c, Gregory A. Neumann b, Carver J. Bierson d, David E. Smith e, Maria T. Zuber e a Department of Geological Sciences, Brown University, Providence, RI 02912, USA b NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA c Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA d Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA 95064, USA e Department of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, MA 02139, USA a r t i c l e i n f o a b s t r a c t Article history: High-resolution gravity data from the Gravity Recovery and Interior Laboratory (GRAIL) mission provide Received 14 September 2016 the opportunity to analyze the detailed gravity and crustal structure of impact features in the morpho- Revised 1 March 2017 logical transition from complex craters to peak-ring basins on the Moon. We calculate average radial Accepted 21 March 2017 profiles of free-air anomalies and Bouguer anomalies for peak-ring basins, protobasins, and the largest Available online 22 March 2017 complex craters. Complex craters and protobasins have free-air anomalies that are positively correlated with surface topography, unlike the prominent lunar mascons (positive free-air anomalies in areas of low elevation) associated with large basins. -
Lunar Club Observations
Guys & Gals, Here, belatedly, is my Christmas present to you. I couldn’t buy each of you a lunar map, so I did the next best thing. Below this letter you’ll find a guide for observing each of the 100 lunar features on the A. L.’s Lunar Club observing list. My guide tells you what the features are, where they are located, what instrument (naked eyes, binoculars or telescope) will give you the best view of them and what you can expect to see when you find them. It may or may not look like it, but this project involved a massive amount of work. In preparing it, I relied heavily on three resources: *The lunar map I used to determine which quadrant of the Moon each feature resides in is the laminated Sky & Telescope Lunar Map – specifically, the one that shows the Moon as we see it naked-eye or in binoculars. (S&T also sells one with the features reversed to match the view in a refracting telescope for the same price.); and *The text consists of information from (a) my own observing notes and (b) material in Ernest Cherrington’s Exploring the Moon Through Binoculars and Small Telescopes. Both the map and Cherrington’s book were door prizes at our Dec. Christmas party. My goal, of course, is to get you interested in learning more about our nearest neighbor in space. The Moon is a fascinating and lovely place, and one that all too often is overlooked by amateur astronomers. But of all the objects in the night sky, the Moon is the most accessible and easiest to observe. -
O Lunar and Planetary Institute Provided by the NASA Astrophysics Data System the BELLS CARBONACEOUS CHONDRITE
BELLS-A CARBONACEOUS CHONDRITE RELATED TO C1 AND C2 CHONDRITES; Andrew M. ~avisland Edward 01sen2. l~amesFranck Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637; 2~epartmentof Geology, Field Museum of Natural History, Chicago, IL 60605. The Bells, Texas meteorite fell on September 9, 1961. It was classified as a Type I1 carbonaceous chondrite by Mason [I]. Bulk samples of Bells have been found to contain 13 to 16 wt% magnetite by magnetic methods [2,3]. This is far more magnetite than is normally found in C2 chondrites and is slightly higher than the levels found in C1 chondrites [3]. McSween and Richardson [41 measured the bulk composition of "matrix" in many carbonaceous chondrites (including Bells) by broad beam electron microprobe analysis. They found a range of compositions among the phyllosilicate matrices of C1 and C2 chond- rites. Bells and the C1 chondrites are at the Fe-poor, Mg- and Si-rich end of this range. McSween [5] point-counted many C2 chondrites and found Bells to be among the most matrix-rich of them. He found a correlation between the composition of matrix and vol% matrix and suggested that increasing degree of alteration of chondrules and inclusions leads to increasing matrix fraction and decreasing Fe content of the matrix. According to his model, Bells should be among the most heavily altered of the C2 chondrites. Until recently, most of the recovered samples of Bells have been in the private collection of Mr. Oscar Monnig and the only sample available for pet- rographic study has been a tiny thin section.