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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. -
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 -
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. -
Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America
Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America There are approximately 101,135sexual abuse claims filed. Of those claims, the Tort Claimants’ Committee estimates that there are approximately 83,807 unique claims if the amended and superseded and multiple claims filed on account of the same survivor are removed. The summary of sexual abuse claims below uses the set of 83,807 of claim for purposes of claims summary below.1 The Tort Claimants’ Committee has broken down the sexual abuse claims in various categories for the purpose of disclosing where and when the sexual abuse claims arose and the identity of certain of the parties that are implicated in the alleged sexual abuse. Attached hereto as Exhibit 1 is a chart that shows the sexual abuse claims broken down by the year in which they first arose. Please note that there approximately 10,500 claims did not provide a date for when the sexual abuse occurred. As a result, those claims have not been assigned a year in which the abuse first arose. Attached hereto as Exhibit 2 is a chart that shows the claims broken down by the state or jurisdiction in which they arose. Please note there are approximately 7,186 claims that did not provide a location of abuse. Those claims are reflected by YY or ZZ in the codes used to identify the applicable state or jurisdiction. Those claims have not been assigned a state or other jurisdiction. Attached hereto as Exhibit 3 is a chart that shows the claims broken down by the Local Council implicated in the sexual abuse. -
Nasa Technical Memorandum Tm-88427 Formation Of
https://ntrs.nasa.gov/search.jsp?R=19860016441 2020-03-20T14:24:06+00:00Z NASA TECHNICAL MEMORANDUM TM-88427 FORMATION OF THE CENTRAL UPLIFT IN METEORIC CRATERS Jvanov, B.A.; Bazilevskiy, A.T.; Sazonova, L.V. Translation of "Ob obrazovanii tsentralnogo podnyatiya v meteoritnykh kraterakh," in "Meteoritika, Akademiya nauk SSSR" No. 40, 1982, pp. 67-81 , f(NASA-TM-88427) FORMATION OF THE CENTBAL N86-25913 DfLIFT IN flETIOEIC CEATEBS {Hatioiial Aeronautics and Space administration) 33 p HC A03/MP A01 CSCX 08G Unclas G3/46 43587 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION WASHINGTON, D.C. 20546 MAY, 1986 FORMATION OF THE CENTRAL UPLIFT IN METEORIC CRATERS V.A. Ivanov INTRODUCTION. /671 Central peaks or central uplifts in meteoric craters are a necessary element in the structure of craters in a certain size range, e.g. craters with a diameter of 25-200 km on the Moon and 4-70 (?) km on Earth. Smaller craters have a simple cup shape; larger craters are complex multiringed structures. The transition from simple cup-shaped craters to craters with central uplifts is associated with a decrease in relative crater depth, which brings into question the depth of excavation during formation of craters with complex structure. A change in crater structure indicates a change in the mechanics of crater formation and requires caution when one attempts to extrapolate to natural occurrences the set of data accumulated during study of this process using experimental explosions and hypervelocity impacts under laboratory conditions. The purpose of this article is to discuss and, if possible, evaluate the relationship of various processes which accompany crater formation; to attempt to identify those which can be related to the natural appearance of central uplifts in impact craters on a certain scale. -
SPS Demos-Cakeraters.Pdf
Cakeraters Demonstration Falling space rocks collide with the surface of planets and moons to create impact craters which can be found all over our solar system Number of Participants: 2-15 Audience: Elementary (ages 5-10) and up Duration: 10-20 mins Difficulty: Level 2 Materials Required: • Brownie or cake mix (darker color preferred) • Baking pan (any appropriate size) • Coffee creamer or any light-colored powder • Hot cocoa mix or any dark-colored powder (Optional) • Phone with slow -motion capabilities (most) • 2.54 cm Ball bearing or equivalent spherical large mass • Rubber band (Optional) Setup: 1. Bake the brownie according to the instructions on the box 2. Once the brownie cools down, take a teaspoonful of the coffee creamer and place it in the center of the uncut brownies. Spread uniformly across an area of 2x the diameter of the ball. 3. Optional: Place a teaspoon full of darker powder on centered on top of the lighter powder. A diameter of approximately the same as the dropped ball is suggested. This will add contrast to the crater patterns generated. Presenter Brief: Be familiar with how craters are formed, and their basic structure. Relate crater structures to experiences student will have had including the moon and when something is dropped in powders or liquid. Explain how meteor size, speed, and angle of incidence affect the way the craters turn out. Understand how tektites are formed. Vocabulary: • Meteors – Space rocks that enter a planet’s atmosphere and burn up at high speeds due to friction with the gases surrounding them. • Asteroids – Small objects made of rocks and metals that were left over from the formation of the solar system. -
Recreation in Idaho: Campgrounds, Sites and Destinations
U.S. Department of the Interior BUREAU OF LAND MANAGEMENT Recreation in Idaho Campgrounds, Sites and Destinations Locations to Explore Four BLM district offices, 12 field offices and the Idaho State Office administer almost 12 million acres of public lands in Idaho. Please reference the colors and map throughout the booklet for specific regions of Idaho. You may also contact our offices with questions or more information. East-Central and Eastern Idaho Northern Idaho BLM IDAHO FALLS DISTRICT BLM COEUR D’ALENE DISTRICT 1405 Hollipark Drive | Idaho Falls, ID 83401 3815 Schreiber Way | Coeur d’Alene, ID 83815 208-524-7500 208-769-5000 BLM Challis Field Office BLM Coeur d’Alene Field Office 721 East Main Avenue, Suite 8 3815 Schreiber Way | Coeur d’Alene, ID 83815 Challis, ID 83226 208-769-5000 208-879-6200 BLM Cottonwood Field Office BLM Pocatello Field Office 2 Butte Drive | Cottonwood, ID 83522 4350 Cliffs Drive | Pocatello, ID 83204 208-962-3245 208-478-6340 Southwestern Idaho BLM Salmon Field Office BLM BOISE DISTRICT 1206 S. Challis St. | Salmon, ID 83467 3948 Development Avenue | Boise, ID 83705 208-756-5400 208-384-3300 BLM Upper Snake Field Office BLM Bruneau Field Office 1405 Hollipark Dr. | Idaho Falls, ID 83401 3948 Development Ave. | Boise, ID 83705 208-524-7500 208-384-3300 South-Central Idaho BLM Four Rivers Field Office and the BLM TWIN FALLS DISTRICT Morley Nelson Snake River Birds of Prey 2536 Kimberly Road | Twin Falls, ID 83301 National Conservation Area 208-735-2060 3948 Development Ave. | Boise, ID 83705 208-384-3300 BLM Burley Field Office 15 East 200 South | Burley, ID 83318 BLM Owyhee Field Office 208-677-6600 20 First Avenue West | Marsing, ID 83639 208-896-5912 BLM Jarbidge Field Office 2536 Kimberly Road | Twin Falls, ID 83301 208-735-2060 BLM Shoshone Field Office including the Craters of the Moon National Monument and Preserve 400 West “F” Street | Shoshone, ID 83352 208-732-7200 Whitewater fun for the family on one of many Idaho rivers. -
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. -
Inspector General
Inspector General Overview The NASA Office of Inspector General (OIG) budget request for FY 2010 is $36.4 million. The NASA OIG consists of 186 auditors, analysts, specialists, investigators, and support staff at NASA Headquarters in Washington, DC, and NASA Centers throughout the United States. The FY 2010 request supports the OIG mission to prevent and detect crime, fraud, waste, abuse, and mismanagement while promoting economy, effectiveness, and efficiency within the Agency. The OIG Office of Audits (OA) conducts independent, objective audits and reviews of NASA and NASA contractor programs and projects to improve NASA operations, as well as a broad range of professional audit and advisory services. It also comments on NASA policies and is responsible for the oversight of audits performed under contract. OA helps NASA accomplish its objectives by bringing a systematic, disciplined approach to evaluate and improve the economy, efficiency, and effectiveness of NASA operations. The OIG Office of Investigations (OI) identifies, investigates, and refers for prosecution cases of crime, waste, fraud, and abuse in NASA programs and operations. The OIG's federal law enforcement officers investigate false claims, false statements, conspiracy, theft, computer crimes, mail fraud, and violations of federal laws, such as the Procurement Integrity Act and the Anti-Kickback Act. Through its investigations, OI also seeks to prevent and deter crime at NASA. NASA's FY 2010 OIG request is broken out as follows: -$30.5 million (84 percent) of the proposed budget is dedicated to personnel and related costs, including salaries, benefits, monetary awards, worker's compensation, permanent change of station costs, as well as the Government's contributions for Social Security, Medicare, health and life insurance, retirement accounts, and matching contributions to Thrift Savings Plan accounts. -
Moon Course Section 27-33 V1.0
Around the Moon in 28 Days: Lunar Observing for Beginners Course Notes Section 27 - Lunar Day 22 Section 28 - Lunar Day 23 Section 29 - Lunar Day 24 Section 30 - Lunar Day 25 Section 31 - Lunar Day 26 Section 32 - Lunar Day 27 Section 33 - Lunar Day 28 (The End) Copyright © 2010 Mintaka Publishing Inc. 2 Section 27 - Lunar Day 22 Tonight's late rising Moon might seem impossible to study when you have a daytime work schedule, but why not consider going to bed early and spending the early morning hours contemplating some lunar history and the peace and quiet before the day begins? Let's journey off to the lonely Riphaeus Mountains just southwest of crater Copernicus. Northeast of the range is another smooth floored area on the border of Oceanus Procellarum. It is here that Surveyor 3 landed on April 19, 1967. Figure 27-1: The major features of the Moon on Day 22 Around the Moon in 28 Days: Lunar Observing for Beginners 3 Figure 27-2: Surveyor 3 and Apollo 12 and 14 landing sites (courtesy of NASA) After bouncing three times, the probe came to rest on a smooth slope in a sub-telescopic crater. As its on-board television monitors watched, Surveyor 3 extended its mechanical arm with a "first of its kind" miniature shovel and dug to a depth of 18 inches. The view of sub-soil material and its clean-cut lines allowed scientists to conclude that the loose lunar soil could compact. Watching Surveyor 3 pound its shovel against the surface, the resulting tiny "dents" answered the crucial question. -
The Geology of Smythii and Marginis
Lunar and Planetary Science XXVIII 1293.PDF THE GEOLOGY OF SMYTHII AND MARIGINIS BASINS USING INTEGRATED REMOTE SENSING TECHNIQUES: A Look At What’s Around The Corner. Jeffrey J. Gillis1, Paul D. Spudis2 and D. Ben J. Bussey2, 1. Dept. of Geology and Geophysics, 6100 South Main Street, MS-126, Rice University, Houston, Texas, 77005. Gil- [email protected] 2. Lunar and Planetary Institute, 3600 Bay Area Blvd., Houston, Texas, 77058. As part of our ongoing study of volcanism on the far side highlands material while craters greater than 350 meters deep of the Moon, we are studying the geologically diverse eastern (e.g. unnamed crater 3.5 km in diameter located at 0.6o N, limb of the Moon. Crustal thickness in this area, 60 - 75 km, 86o E) have excavated highlands material from beneath the [1, 2] approximates more closely the average crustal thick- mare. Thus, we estimate that the basalt is approximately 325 ness of the far side of the Moon (100 km) than the crustal meters thick at most. thickness beneath the near side, Apollo sites (40-60 km). Moreover, the eastern limb region has been documented by a A unit with intermediate albedo and iron values (10 - 12 wt. variety of remote sensing techniques: Lunar Orbiter and % FeO) occupies the southwestern central area of the Apollo images, Apollo X-ray and gamma-ray data, and Smythii basin. Topographically higher, this unit forms an Clementine gravity, topography and multispectral images. elongate arch that stretches from northwest to southeast and divides the main basalt deposit to the northeast from two A comprehensive study of the geology of the eastern limb of isolated basalt patches to the south and southwest.