Ice& Stone 2020
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
China's Touch on the Moon
commentary China’s touch on the Moon Long Xiao As well as being a milestone in technology, the Chang’e lunar exploration programme establishes China as a contributor to space science. With much still to learn about the Moon, fieldwork beyond Earth’s orbit must be an international effort. hen China’s Chang’e 3 spacecraft geological history of the landing site. touched down on the lunar High-resolution images have shown rocky Wsurface on 14 December 2013, terrain with outcrops of porphyritic basalt, it was the first soft landing on the Moon such as Loong Rock (Fig. 2). Analysis since the Soviet Union’s Luna 24 mission of data collected by the penetrating in 1976. Following on from the decades- Chang’e 3 radar should lead to identification of the old triumphs of the Luna missions and underlying layers of regolith, impact breccia NASA’s Apollo programme, the Chang’e and basalt. lunar exploration programme is leading the China’s robotic field geologist Yutu has charge of a new generation of exploration Basalt outcrop Yutu rover stalled in its traverse of the lunar surface, on the lunar surface. Much like the earlier but plans for the Chang’e 5 sample-return space programmes, the China National mission are moving forward. The primary Space Administration (CNSA) has been objective of the mission will be to return developing its capabilities and technologies 100 m 2 kg of samples from the surface and depths step by step in a series of Chang’e missions UNIVERSITY STATE © NASA/GSFC/ARIZONA of up to 2 m, probably also in the relatively of increasing ambition: orbiting and Figure 1 | The Chinese Chang’e 3 spacecraft and smooth northern Mare Imbrium. -
Untangling the Formation and Liberation of Water in the Lunar Regolith
Untangling the formation and liberation of water in the lunar regolith Cheng Zhua,b,1, Parker B. Crandalla,b,1, Jeffrey J. Gillis-Davisc,2, Hope A. Ishiic, John P. Bradleyc, Laura M. Corleyc, and Ralf I. Kaisera,b,2 aDepartment of Chemistry, University of Hawai‘iatManoa, Honolulu, HI 96822; bW. M. Keck Laboratory in Astrochemistry, University of Hawai‘iatManoa, Honolulu, HI 96822; and cHawai‘i Institute of Geophysics and Planetology, University of Hawai‘iatManoa, Honolulu, HI 96822 Edited by Mark H. Thiemens, University of California at San Diego, La Jolla, CA, and approved April 24, 2019 (received for review November 15, 2018) −8 −6 The source of water (H2O) and hydroxyl radicals (OH), identified between 10 and 10 torr observed either an ν(O−H) stretching − − on the lunar surface, represents a fundamental, unsolved puzzle. mode in the 2.70 μm (3,700 cm 1) to 3.33 μm (3,000 cm 1) region The interaction of solar-wind protons with silicates and oxides has exploiting infrared spectroscopy (7, 25, 26) or OH/H2Osignature been proposed as a key mechanism, but laboratory experiments using secondary-ion mass spectrometry (27) and valence electron yield conflicting results that suggest that proton implantation energy loss spectroscopy (VEEL) (28). However, contradictory alone is insufficient to generate and liberate water. Here, we dem- studies yielded no evidence of H2O/OH in proton-bombarded onstrate in laboratory simulation experiments combined with minerals in experiments performed under ultrahigh vacuum − − imaging studies that water can be efficiently generated and re- (UHV) (10 10 to 10 9 torr) (29). -
Exploration of the Moon
Exploration of the Moon The physical exploration of the Moon began when Luna 2, a space probe launched by the Soviet Union, made an impact on the surface of the Moon on September 14, 1959. Prior to that the only available means of exploration had been observation from Earth. The invention of the optical telescope brought about the first leap in the quality of lunar observations. Galileo Galilei is generally credited as the first person to use a telescope for astronomical purposes; having made his own telescope in 1609, the mountains and craters on the lunar surface were among his first observations using it. NASA's Apollo program was the first, and to date only, mission to successfully land humans on the Moon, which it did six times. The first landing took place in 1969, when astronauts placed scientific instruments and returnedlunar samples to Earth. Apollo 12 Lunar Module Intrepid prepares to descend towards the surface of the Moon. NASA photo. Contents Early history Space race Recent exploration Plans Past and future lunar missions See also References External links Early history The ancient Greek philosopher Anaxagoras (d. 428 BC) reasoned that the Sun and Moon were both giant spherical rocks, and that the latter reflected the light of the former. His non-religious view of the heavens was one cause for his imprisonment and eventual exile.[1] In his little book On the Face in the Moon's Orb, Plutarch suggested that the Moon had deep recesses in which the light of the Sun did not reach and that the spots are nothing but the shadows of rivers or deep chasms. -
Contributions of a Lunar Geoscience Observer (Lgo) Mission to Fundamental Questions in Lunar Science
CONTRIBUTIONS OF A LUNAR GEOSCIENCE OBSERVER (LGO) MISSION TO FUNDAMENTAL QUESTIONS IN LUNAR SCIENCE by LGO SCIENCE WORKSHOP MEMBERS Contributions Lunar Geoscience Observer Mission Frontispiece: Earth-rise over the lunar highlands. Contributions of a Lunar Geoscience Observer Mission to Fundaments Questions in Lunar Science LGO Science Workshop Members March LGO Science Workshop Members Roger Phillips (Chair), Southern Methodist University Merton Davies, Rand Coworation Michael Drake, University of Arizona Michael Duke, Johnson Space Center Larry Haskin. Washington University James Head, Brown University Eon Mood, University of Arizona Robert Lin, University of California, Berkeley Duane Muhleman, California Institute of Technology Doug Nash (Study Scientist), Jet Propulsion Laboratory Carle Pieters, Brown University Bill Sjogren, Jet Propulsion Laboratory Paul Spudis, U .S. Geological Survey Jeff Taylor, University of New Mexico Jacob Trombka, Goddard Space Flight Center This report was compiled and prepared in the Department of Geological Sciences and the AnthroGraphics Laboratory of Southern Methodist University. Material in this document may be copied without restraint for library, abstract service, educational or personal research purposes. Republication of any portion should be accompanied by the appropriate acknowledgment of this document. For further information, contact: Dr. Roger Phillips Department of Geological Sciences Southern Methodist University Dallas, TX 75275 Executive Summary THE IMPORTANCE OF LUNAR SCIENCE STATUS OF LUNAR SCIENCE DATA AND THEORY The Moon is the keystone in the interlinked knowledge that forms the foundation of our understanding of the silicate Unlike other solar system bodies beyond Earth, the Moon bodies of the solar system. The Moon is remarkable in that it has been intensely studied by telescope, unmanned space- remains the only other planet for which we have samples of crafi and manned missions. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
MODELING and SIMULATION of the CHANDRAYAAN-I HYSI DATA for MINERAL MIXING ANALYSIS. S.B. Sayyad and Mohammed Zeeshan R, (Departm
4th Planetary Data Workshop 2019 (LPI Contrib. No. 2151) 7074.pdf MODELING AND SIMULATION OF THE CHANDRAYAAN-I HYSI DATA FOR MINERAL MIXING ANALYSIS. S.B. Sayyad and Mohammed Zeeshan R, (Department of Physics, Milliya College Arts Science and Management Science College Beed Maharashtra India. [email protected], [email protected] ) Introduction: The space weathering is the primary process involved on the lunar surface which has the strong influence on the reflectance properties because of the accumulation of small submicroscopic iron [1- 2]. Long time exposure to the environment complicates the understanding of the surface composition [3-6] Theoretical model can be employed to understand the effect of space weathering and to study the composition of the lunar regolith. From the studies done on the lu- nar samples from the Apollo mission it was clear that there are the significant differences between the optical properties of spectra pulverized in the laboratory and spectra obtained from the lunar soil [7-9]. The lunar Fig. 1. Site Location of Mare Crisium and data subset of soil spectra shows systematic influence of space weath- Mare Crisium. ering which is reduction in overall reflectance red- dened -slope continuum and attenuated absorption bands. To model the measured reflectance spectra of Chandrayaan-1 hyperspectral Imager (HySI) we have obtained an artificial reflectance spectrum using Bi- directional reflectance function (BRDF) based on the equation of radiative transfer proposed by Bruce Hap- ke and published in the series of papers [10-14]. The effect of space weathering, particle size, single particle phase function, porosity can be easily accommodated and it is con- sidered to be most efficient for modeling asteroids and plane- tary surfaces Modeling the Chandrayaan-1 HySI dataset: The Band to band registered level-4 HySI image was Fig.2. -
Surveyor 1 Space- Craft on June 2, 1966 As Seen by the Narrow Angle Camera of the Lunar Re- Connaissance Orbiter Taken on July 17, 2009 (Also See Fig
i “Project Surveyor, in particular, removed any doubt that it was possible for Americans to land on the Moon and explore its surface.” — Harrison H. Schmitt, Apollo 17 Scientist-Astronaut ii Frontispiece: Landing site of the Surveyor 1 space- craft on June 2, 1966 as seen by the narrow angle camera of the Lunar Re- connaissance Orbiter taken on July 17, 2009 (also see Fig. 13). The white square in the upper photo outlines the area of the enlarged view below. The spacecraft is ca. 3.3 m tall and is casting a 15 m shadow to the East. (NASA/LROC/ ASU/GSFC photos) iii iv Surveyor I: America’s First Moon Landing by William F. Mellberg v © 2014, 2015 William F. Mellberg vi About the author: William Mellberg was a marketing and public relations representative with Fokker Aircraft. He is also an aerospace historian, having published many articles on both the development of airplanes and space vehicles in various magazines. He is the author of Famous Airliners and Moon Missions. He also serves as co-Editor of Harrison H. Schmitt’s website: http://americasuncommonsense.com Acknowledgments: The support and recollections of Frank Mellberg, Harrison Schmitt, Justin Rennilson, Alexander Gurshstein, Paul Spudis, Ronald Wells, Colin Mackellar and Dwight Steven- Boniecki is gratefully acknowledged. vii Surveyor I: America’s First Moon Landing by William F. Mellberg A Journey of 250,000 Miles . December 14, 2013. China’s Chang’e 3 spacecraft successfully touched down on the Moon at 1311 GMT (2111 Beijing Time). The landing site was in Mare Imbrium, the Sea of Rains, about 25 miles (40 km) south of the small crater, Laplace F, and roughly 100 miles (160 km) east of its original target in Sinus Iridum, the Bay of Rainbows. -
Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa
dsc_cover (Converted)-1 8/6/02 10:33 AM Page 1 Deep Space Chronicle Deep Space Chronicle: A Chronology ofDeep Space and Planetary Probes, 1958–2000 |Asif A.Siddiqi National Aeronautics and Space Administration NASA SP-2002-4524 A Chronology of Deep Space and Planetary Probes 1958–2000 Asif A. Siddiqi NASA SP-2002-4524 Monographs in Aerospace History Number 24 dsc_cover (Converted)-1 8/6/02 10:33 AM Page 2 Cover photo: A montage of planetary images taken by Mariner 10, the Mars Global Surveyor Orbiter, Voyager 1, and Voyager 2, all managed by the Jet Propulsion Laboratory in Pasadena, California. Included (from top to bottom) are images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus, and Neptune. The inner planets (Mercury, Venus, Earth and its Moon, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. NASA SP-2002-4524 Deep Space Chronicle A Chronology of Deep Space and Planetary Probes 1958–2000 ASIF A. SIDDIQI Monographs in Aerospace History Number 24 June 2002 National Aeronautics and Space Administration Office of External Relations NASA History Office Washington, DC 20546-0001 Library of Congress Cataloging-in-Publication Data Siddiqi, Asif A., 1966 Deep space chronicle: a chronology of deep space and planetary probes, 1958-2000 / by Asif A. Siddiqi. p.cm. – (Monographs in aerospace history; no. 24) (NASA SP; 2002-4524) Includes bibliographical references and index. 1. Space flight—History—20th century. I. Title. II. Series. III. NASA SP; 4524 TL 790.S53 2002 629.4’1’0904—dc21 2001044012 Table of Contents Foreword by Roger D. -
Scientists Finds Evidence of Water Ice on Asteroid's Surface 28 April 2010
Scientists finds evidence of water ice on asteroid's surface 28 April 2010 Johns Hopkins University in Laurel, Md., examined the surface of 24 Themis, a 200-kilometer wide asteroid that sits halfway between Mars and Jupiter. By measuring the spectrum of infrared sunlight reflected by the object, the researchers found the spectrum consistent with frozen water and determined that 24 Themis is coated with a thin film of ice. They also detected organic material. "The organics we detected appear to be complex, long-chained molecules. Raining down on a barren Earth in meteorites, these could have given a big kick-start to the development of life," Emery said. Emery noted that finding ice on the surface of 24 Themis was a surprise because the surface is too warm for ice to stick around for a long time. This image shows the Themis Main Belt which sits between Mars and Jupiter. Asteroid 24 Themis, one of "This implies that ice is quite abundant in the the largest Main Belt asteroids, was examined by interior of 24 Themis and perhaps many other University of Tennessee scientist, Josh Emery, who asteroids. This ice on asteroids may be the answer found water ice and organic material on the asteroid's to the puzzle of where Earth's water came from," he surface. His findings were published in the April 2010 said. issue of Nature. Credit: Josh Emery/University of Tennessee, Knoxville Still, how the water ice got there is unclear. 24 Themis' proximity to the sun causes ice to vaporize. However, the researchers' findings Asteroids may not be the dark, dry, lifeless chunks suggest the asteroid's lifetime of ice ranges from of rock scientists have long thought. -
SOFIA Successfully Completes
June 2010 - A Quarterly Publication SOFIA successfully completes its ‘first light’ flight BY CATHY WESELBY The Stratospheric Observatory for Infrared Astronomy, or SOFIA, achieved a major milestone May 26, with its first in-flight night observations. Astronomers call this event for a new observatory “first light.” The highly modified Boeing 747SP jetliner fitted with a 100-inch diameter reflecting telescope took off from its home base at the Aircraft Operations Anthony Wesley photo by NASA Facility in Palmdale, Calif., of NASA's Dryden Flight Research Center. The in-flight personnel consisted of an international crew from NASA, the Universities Space Research Associa- tion in Columbia, Md., Cornell Univer- sity and the German SOFIA Institute (DSI) in Stuttgart. During the six-hour This composite infrared image of Jupiter was made by Cornell University’s FORCAST camera flight, at altitudes up to 35,000 feet, during the SOFIA observatory’s "first light" flight. A recent visual-wavelength picture of approxi- the crew of 10 scientists, astronomers, mately the same side of Jupiter is shown for comparison. engineers and technicians gathered We’re back! By popular demand, the Astro- gram is resuming publication this month as a quarterly newsletter. It will be available online and in hard- NASA photo by Jim Ross NASA copy format and mailed to onsite mailstops and Ames retirees. The Astrogram will be published every three months. The Astrogram will be available online at http://www.nasa. gov/centers/ames/news/astrogram/ index.html Ames Public Affairs is soliciting Its primary mirror covered by a protective sun shade, the German-built infrared telescope short articles (600 word maximum) nestled in the rear fuselage of NASA's SOFIA flying observatory is easily visible in this close- up image taken during a recent test flight. -
Hydrated Minerals on Asteroids: the Astronomical Record
Hydrated Minerals on Asteroids: The Astronomical Record A. S. Rivkin, E. S. Howell, F. Vilas, and L. A. Lebofsky March 28, 2002 Corresponding Author: Andrew Rivkin MIT 54-418 77 Massachusetts Ave. Cambridge MA, 02139 [email protected] 1 1 Abstract Knowledge of the hydrated mineral inventory on the asteroids is important for deducing the origin of Earth’s water, interpreting the meteorite record, and unraveling the processes occurring during the earliest times in solar system history. Reflectance spectroscopy shows absorption features in both the 0.6-0.8 and 2.5-3.5 pm regions, which are diagnostic of or associated with hydrated minerals. Observations in those regions show that hydrated minerals are common in the mid-asteroid belt, and can be found in unex- pected spectral groupings, as well. Asteroid groups formerly associated with mineralogies assumed to have high temperature formation, such as MAand E-class asteroids, have been observed to have hydration features in their reflectance spectra. Some asteroids have apparently been heated to several hundred degrees Celsius, enough to destroy some fraction of their phyllosili- cates. Others have rotational variation suggesting that heating was uneven. We summarize this work, and present the astronomical evidence for water- and hydroxyl-bearing minerals on asteroids. 2 Introduction Extraterrestrial water and water-bearing minerals are of great importance both for understanding the formation and evolution of the solar system and for supporting future human activities in space. The presence of water is thought to be one of the necessary conditions for the formation of life as 2 we know it. -
Asteroid Photometric and Polarimetric Phase Curves: Joint Linear-Exponential Modeling
Meteoritics & Planetary Science 44, Nr 12, 1937–1946 (2009) Abstract available online at http://meteoritics.org Asteroid photometric and polarimetric phase curves: Joint linear-exponential modeling K. MUINONEN1, 2, A. PENTTILÄ1, A. CELLINO3, I. N. BELSKAYA4, M. DELBÒ5, A. C. LEVASSEUR-REGOURD6, and E. F. TEDESCO7 1University of Helsinki, Observatory, Kopernikuksentie 1, P.O. BOX 14, FI-00014 U. Helsinki, Finland 2Finnish Geodetic Institute, Geodeetinrinne 2, P.O. Box 15, FI-02431 Masala, Finland 3INAF-Osservatorio Astronomico di Torino, strada Osservatorio 20, 10025 Pino Torinese, Italy 4Astronomical Institute of Kharkiv National University, 35 Sumska Street, 61035 Kharkiv, Ukraine 5IUMR 6202 Laboratoire Cassiopée, Observatoire de la Côte d’Azur, BP 4229, 06304 Nice, Cedex 4, France 6UPMC Univ. Paris 06, UMR 7620, BP3, 91371 Verrières, France 7Planetary Science Institute, 1700 E. Ft. Lowell Road, Tucson, Arizona 85719, USA *Corresponding author. E-mail: [email protected] (Received 01 April, 2009; revision accepted 18 August 2009) Abstract–We present Markov-Chain Monte-Carlo methods (MCMC) for the derivation of empirical model parameters for photometric and polarimetric phase curves of asteroids. Here we model the two phase curves jointly at phase angles գ25° using a linear-exponential model, accounting for the opposition effect in disk-integrated brightness and the negative branch in the degree of linear polarization. We apply the MCMC methods to V-band phase curves of asteroids 419 Aurelia (taxonomic class F), 24 Themis (C), 1 Ceres (G), 20 Massalia (S), 55 Pandora (M), and 64 Angelina (E). We show that the photometric and polarimetric phase curves can be described using a common nonlinear parameter for the angular widths of the opposition effect and negative-polarization branch, thus supporting the hypothesis of common physical mechanisms being responsible for the phenomena.