DOCSLIB.ORG

Brightness Temperatures of the Lunar Surface: the Clementine Long-Wave Infrared Global Data Set

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Brightness Temperatures of the Lunar Surface: the Clementine Long-Wave Infrared Global Data Set Lunar and Planetary Science XXX 1892.pdf BRIGHTNESS TEMPERATURES OF THE LUNAR SURFACE: THE CLEMENTINE LONG-WAVE INFRARED GLOBAL DATA SET. S. L. Lawson and B. M. Jakosky, Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392 ([email protected]). Introduction: Observers have been measuring the with emissivity e, Stefan-Boltzmann constant s, MoonÕs thermal emission for many years [1, 2, 3, 4]. albedo A, solar constant So, and Sun-Moon distance R In 1930, Pettit and Nicholson first measured the full in AU. Assuming unit emissivity, the Lambertian Moon surface emission to be non-Lambertian [1]. They temperature T is the temperature of a black body found the temperature along the lunar equator radiating the same power that is absorbed from the empirically varied as cos1/6(i), as opposed to the Sun. cos1/4(i) variation expected from a Lambertian surface; Figure 1 shows a comparison of LWIR data with the temperature away from the subsolar point decreased calculated Lambertian temperatures as a function of more slowly than would be expected from a latitude. The variation of brightness temperature as Lambertian surface. In the 1960s, Sinton [3] measured cos1/6(i) is also plotted. The data points in Figure 1 are the subsolar point brightness over a lunation and also LWIR image-averaged temperatures for ten Clementine found that the angular brightness dependence was not orbits (152-156 and 168-172) where the Sun was that of a spherical Lambertian surface. Both these within one degree of local noon (i » latitude). No observations have been interpreted as an effect of assumptions about lunar surface thermal properties average lunar surface roughness. The limb of the full were made when reducing the plotted LWIR data. The Moon is brighter than that expected from a smooth red (upper) line represents the cos1/6(i) temperature surface because the randomly oriented surfaces of rough variation of Pettit and Nicholson [1], whereas the green particles radiate more efficiently in the direction of the (lower) line shows the Lambertian temperature observer than a similar smooth surface would. We find variation of cos1/4(i). The 2s errors for the LWIR data that nadir-looking observations of the lunar surface do are approximately 8 K near the equator and increase to not exhibit this anomalous behavior, but instead vary over 40 K at high latitudes. as cos1/4(i). The scientific payload on the Clementine spacecraft included a Long-Wave Infrared (LWIR) camera with a single passband of width 1.5 mm centered at a wavelength of 8.75 mm. The Clementine orbit deviated ±30û from sun synchronous, and for two lunar months dayside nadir-looking images were obtained near local noon [5]. Contiguous pole-to-pole imaging strips were obtained with approximately 10% overlap between adjacent frames. However, significant longitude gaps exist between successive orbital passes. During the systematic mapping phase of the Clementine mission, approximately 220,000 thermal-infrared images of the lunar surface were obtained. Observed LWIR radiances can be converted to brightness temperatures which provide information on various physical properties of Figure 1. LWIR image-averaged temperatures and the lunar surface. equilibrium models as a function of latitude. For the Analysis: A simple thermal equilibrium model models, i = latitude, e = 1, A = 0.15, and R = 1 AU. was used to calculate expected brightness temperatures of the lunar surface. Because the lunar surface layer is Discussion: The albedo used for the model highly insulating and the LWIR observations were temperatures in Figure 1 is 0.15, which is a highlands very near local noon, conduction into the regolith was average. The longitude ranges for the Clementine neglected. The Moon was assumed to be a smooth orbits plotted in Figure 1 are 350û-5û and 30û-45û. At spherical object in instantaneous equilibrium with the these longitudes, there are maria at mid-latitudes. solar insolation, and the local temperature T varied Since maria have lower albedos than highlands (values with solar incidence angle i as: typically ranging from 0.07 to 0.10), it is expected that 14/ TT= cos ( i ). the equatorial data in Figure 1 are warmer than the SS The subsolar temperature T was calculated from models. It is clear from Figure 1 that the LWIR SS temperatures do not follow a cos1/6(i) temperature 4 S o variation, but instead are well fit by the Lambertian esTA=-()1 SS 2 temperature model. This is expected due to the fact R that the LWIR observations are nadir-looking, where Lunar and Planetary Science XXX 1892.pdf BRIGHTNESS TEMPERATURES OF THE LUNAR SURFACE: S. L. Lawson and B. M. Jakosky the effects of surface relief average out over a single due to the large errors there. Figure 2 clearly shows frame. A cratered surface may appear warmer than a that the Moon is hotter at the equator than it is at the smooth surface when viewed from overhead during the poles. Many lunar features stand out in Figure 2, such lunar day. In addition, a surface with rocks may appear as Mare Orientale, Mare Crisium, and the Apennine cooler than a smooth surface. These two effects on Mountains. At equatorial latitudes, the nearside maria observed temperature can be thought to cancel when are warmer than the farside highlands. Figure 2 positive and negative relief are viewed together from demonstrates that the dayside lunar thermal emission overhead. is largely governed by albedo and by the intensity of Figure 1 demonstrates that a Lambertian surface is solar radiation. adequate for modeling nadir-looking temperature Conclusions: The LWIR data from noontime observations of the lunar surface. The LWIR data were orbits demonstrate that the Lambertian temperature observed at incidence angles of ±30û from local noon, model of cos1/4(i) is a fair approximation for nadir- and at different Sun-Moon distances. Thus, in order to looking temperatures. Deviations from the Lambertian compare LWIR data from all of the Clementine orbits model are likely due to surface roughness effects and we used the following formulation: variations in infrared emissivity. In addition, the 2 LWIR global data set reveal the dayside lunar thermal 44 cos(inoon ) Rmeasured emission to be largely governed by albedo, by the TT= , noon measured 2 intensity of solar radiation, and by the emission angle cos(imeasured ) R noon of observations. where inoon is the image latitude minus the latitude of References: [1] Pettit, E. and S.ÊB. Nicholson the sub-solar point and Rnoon is 1 AU. Clementine (1930). Astrophys. J. 71, 102-135. [2] Sinton, W. month 2 data was multiplied by a scale factor, but the (1962). Chapter 11 in Physics and Astronomy of the resulting temperatures remained within the 2s errors. Moon, ed. Kopal. [3] Saari, J.ÊM. and R.ÊW. Shorthill Figure 2 shows the LWIR image-averaged (1972). Moon 5, 161-178. [4] Mendell, W.ÊW. and temperatures adjusted to local noon and interpolated F.ÊJ. Low (1975). Proc. Lunar Sci. Conf. 6th, 2711- onto a new grid of one square degree intervals. Data 2883. [5] Nozette, S., et al. (1994). Science 266, gaps (longitudinal stripes) were filled via a simple 1835-1839. smoothing routine and high latitudes were neglected Figure 2. LWIR global mosaic of image-averaged temperatures adjusted to local noon, interpolated onto a new grid of one square degree intervals, and smoothed over longitudinal gaps..
Load more

Recommended publications
  • Martian Crater Morphology
    ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter.
    [Show full text]
  • The Surface of the Moon
    THE SURFACE OF THE MOON OBSERVATIONS BY THE COMMITTEE ON STUDY OF THE SURFACE FEATURES OF THE MOON F. E. WRIGHT Geophysical Laboratory HE 'I'he Carnegie Institution of Washington Carnegie Institution of Washington was founded by TAndrew Carnegie to advance knowledge in different fields of science through research work. In the early days of the Institution careful surveys of certain branches of sciences were made by special committees of experts to ascertain the particular problems in each field that were strategically important and could be attacked by scientists working together but approaching each problem from different standpoints. The value of diversified but coordinated attack on a problem is well recognized in the military services (tactics) and is equally important in science. The committees, after study of the different fields, recommended certain problems for consideration. Of these a limited number were adopted and small groups of research men were brought to­ gether and given opportunity to work on them. These groups were gradually organized into the departments and laboratories of the Institution. A number of these units have now been operating for more than thirty years, and have made extremely important contributions to science. In addition to support of the work of the departments, the Institution has aided many individual inves­ tigators (research associates) on specific problems related to work of the Institution. During the first twenty years of their existence the departments were so occupied with their own problems that each one functioned as an independent unit with little knowledge of the work and per­ sonnel of the other groups.
    [Show full text]
  • I B R EL ORNIA
    i • a _' a SPACE SCIENCES LABORATORY I # # i UNIVERSITY CALIFORNIA i B_R_EL ORNIA : NRT- o62_o r , - o / - . -.- L (NASA. CR OR TMX OR Ai2 NUMBER) |CATRGORY) 4 3 ,.. -. , , "I Space Science_ Lal_oratory W University of California Berkeley, California 94720 0 RADIATION ANOMALIES ON THE LUNAR SURFACE by David Buhl A Technical Report on NASA Grants NsG 101-61 and NsG Z43-6Z Series No. 8, Issue No. 1 Submitted in partial satisfaction of the requirements for the degree of DOCTOR OF PHILOSOPHY Department of Electrical Engineering University of California, Berkeley t January20, 1967 0 8 * 4 r B CONTENTS ABSTRACT ............................. vii ACKNOWLEDGMENTS ....................... _x I • INTRODUCTION ........................... I II. PROPOSAL -- A Study of the Eff;cts of Luna: Cratering on Infrared Observations ............... III. THEORETICAL ANAL _SiS .......... .......... I_ I. Model of a Cra_ered Lunar Surface .............. i8 i. 1 Description nf a model lunar c"ater ............ l_ 1.2 Asstlmp ions made concerning the surface of a crater . ZI i. 3 Consideration of radiation and re radiation in lunar crater 24 1.4 Density nf lunar craters .................. 27 0 Z. Mathematic Aralysis of the Temperature Eistribution ..... _8 2.1 The integral equation for a sl)eric_l crater ........ _8 2.2 Equations describing the temperat;are history of a crater 35 3. Daytime Study of the Moon .................... 42 3.1 The experiments of Pettit and Nicholson ......... 42 3.2 The temperature distribution in an illuminated crater . 44 3.3 The shadow region of a crater ............. 46 3.4 The angular distribution of radiation from a crater . 4q 3.5 _adiation patterns of several craters ..........
    [Show full text]
  • Annual Progress Report
    ? ASTRDGEOLOGIC ANNUAL PROGRESS REPORT July 1, 1964 to c July 1, 1965 xov&iiib&r1365 This preliminary report is distributed without editorial and technical review for conformity with official standards and nomenclature. It should not be quoted without permission. This report concerns work done on behalf of the National Aeronautics and Space Administration. DEPARTMENT OF THE INTERIOR UNITED STATES GEOIX)(;ICAL SURVEY 6 F DISTRIBUTION No. of Copies National Aeronautics and Space Administration Washington, D.C. ......................... -20 U.S. Geological Survey ...................... .10 A'~elsoii, Dr. P. E., Oirector Geophysical Laboratory Carnegie Institution Washington, D.C. .......................... 1 Allen, Mr. H. J. Ames Research Center Moffett Field, California. ..................... 1 Babcock, Dr. H. W., Director Mt. Wilson and Palomar Observatories Mount Wilson, California ...................... 1 Beattie, Mr. D. A. National Aeronautics and Space Administration Washington, D.C. ......................... .1 Brown, Professor Harrison Division of Geological Sciences California Institute of Technology Pasadena, California ........................ 1 Bryson, Mr. R. P. National Aeronautics and Space Administration Washington, D.C. .......................... 2 Cannell, Mr. W. D. Aeronautical Chart and Information Center Lowell Observatory Flagstaff, Arizona ......................... 1 Carder, Mr. R. W. Aeronautical Chart and Information Center Second and Arsenal Streets St. Louis, Missouri. ........................ 1 Chapman, 'Dr. D.
    [Show full text]
  • Mare Moscoviense
    80°E 90°E 100°E 110°E 120°E 130°E 140°E 150°E 160°E 170°E 180° 170°W 160°W 150°W 140°W 130°W 120°W 110°W 100°W 90°W 80°W 50°N 50°N Chapman Paraskevopoulos De Moraes D'Alembert Galvani Debye Sarton Slipher Esnault-Pelterie Montgolfier Chernyshev Schlesinger d . Segers Perkin McLaughlin ar Millikan Rynin Stefan Ger ae Boss Petrie Campbell Guillaume Rim Woltjer . Wegener . Stoletov . Rayet Dunér Gullstrand Schönfeld Pawsey Langevin . Chandler Wood Gerard Vashakidze Bridgman Quetelet Fabry Ley . Winkler Von Zeipel . Becquerel Kulik Fowler Landau Bragg Schneller Perrine Lacchini Bunsen . Sisakyan Wiener H. G. Wells . Ehrlich Von Neumann Thiel 40°N . 40°N Golovin Avicenna Riemann C Razumov a Harkhebi te n Cantor a Tesla Kurchatov Cate Lavoisier na Champollion S K um ur Sumner n cha . er to Frost Beals v Appleton Hutton Moore Parsons Klute . Petropavlovskiy . Giordano Bruno Van Gadomski Charlier Gauss Kidinnu Maanen Douglass Nernst Krylov Evershed Winlock . Nikolaev . Evdokimov Stearns Vestine Szilard Hogg Harriot . Steno Lorentz Röntgen Aston Ulugh Richardson Nijland Sanford Healy v Beigh Nusl Shayn Larmor Teisserenc Blazhko Cockcroft Van den . Feoktistov Bergh Kovalevskaya Maxwell 30°N 30°N Rayleigh Trumpler . Hatanaka Leucippus Seyfert . Kepínski Titov . Tereshkova Espin Innes Laue Urey . Voskresenskiy Catena Ar Lomonosov Fitzgerald Joule . Seneca MARE . Bobone Lyapunov . tamono Parenago Artamonov Bronk Joliot Polzunov Florensky MOSCOVIENSE Dante Ingalls v Komarov Edison Tikhomirov Berkner Freundlich Mineur Bartels Deutsch Meggers . Shatalov Comrie Belyaev Foster . McNally Vernadskiy . Marci Hubble Morse Jackson Helberg Malyy Siedentopf Comstock Robertson Bell Buys- Dziewulski Moseley Olcott Ballot Nagaoka 20°N Catena Dzie .
    [Show full text]
  • Edison Pettit Papers: Finding Aid
    http://oac.cdlib.org/findaid/ark:/13030/tf9q2nb3w2 No online items Edison Pettit Papers: Finding Aid Processed by Ronald S. Brashear in March 1998. The Huntington Library, Art Collections, and Botanical Gardens Manuscripts Department 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2191 Email: [email protected] URL: http://www.huntington.org © 1998 The Huntington Library. All rights reserved. Edison Pettit Papers: Finding Aid mssPettit papers 1 Overview of the Collection Title: Edison Pettit Papers Dates (inclusive): 1920-1969 Collection Number: mssPettit papers Creator: Pettit, Edison, 1889-1962. Extent: 6 boxes (3,100 pieces) Repository: The Huntington Library, Art Collections, and Botanical Gardens. Manuscripts Department 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2191 Email: [email protected] URL: http://www.huntington.org Abstract: This collection contains the papers of astronomer Edison Pettit (1889-1962), who was on the staff of the Mount Wilson and Palomar Observatories. The correspondence is chiefly with other astronomers in the United States and deals with astronomy in general including Pettit's work at Mount Wilson, telescopes, and ultraviolet light research. The rest of the collection is made up of manuscripts, notes, notebooks and printed items. Language: English. Access Open to qualified researchers by prior application through the Reader Services Department. For more information, contact Reader Services. Publication Rights The Huntington Library does not require that researchers request permission to quote from or publish images of this material, nor does it charge fees for such activities. The responsibility for identifying the copyright holder, if there is one, and obtaining necessary permissions rests with the researcher.
    [Show full text]
  • Observing the Lunar Libration Zones
    Observing the Lunar Libration Zones Alexander Vandenbohede 2005 Many Look, Few Observe (Harold Hill, 1991) Table of Contents Introduction 1 1 Libration and libration zones 3 2 Mare Orientale 14 3 South Pole 18 4 Mare Australe 23 5 Mare Marginis and Mare Smithii 26 6 Mare Humboldtianum 29 7 North Pole 33 8 Oceanus Procellarum 37 Appendix I: Observational Circumstances and Equipment 43 Appendix II: Time Stratigraphical Table of the Moon and the Lunar Geological Map 44 Appendix III: Bibliography 46 Introduction – Why Observe the Libration Zones? You might think that, because the Moon always keeps the same hemisphere turned towards the Earth as a consequence of its captured rotation, we always see the same 50% of the lunar surface. Well, this is not true. Because of the complicated motion of the Moon (see chapter 1) we can see a little bit around the east and west limb and over the north and south poles. The result is that we can observe 59% of the lunar surface. This extra 9% of lunar soil is called the libration zones because the motion, a gentle wobbling of the Moon in the Earth’s sky responsible for this, is called libration. In spite of the remainder of the lunar Earth-faced side, observing and even the basic task of identifying formations in the libration zones is not easy. The formations are foreshortened and seen highly edge-on. Obviously, you will need to know when libration favours which part of the lunar limb and how much you can look around the Moon’s limb.
    [Show full text]
  • Physics of the Moon
    NASA TECHNICAL NOTE -cNASA TN D-2944 e. / PHYSICS OF THE MOON SELECTED TOPICS CONCERNING LUNAR EXPLORATION Edited by George C. ‘Bucker and Henry E. Siern George C. Marsball Space Flight Center Hzmtsville, A Za: NATIONAL AERONAUTICSAND SPACEADMINISTRATION - WASHINGTON;D. C. TECH LIBRARY KAFB. NM llL5475b NASA TN D-2944 PHYSICS OF THE MOON SELECTED TOPICS CONCERNING LUNAR EXPLORATION Edited by George C. Bucher and Henry E. Stern George C. Marshall Space Flight Center Huntsville, Ala. NATIONAL AERONAUTICS AND SPACE ADMINISTRATION For sole by the Clearinghouse for Federal Scientific and Technical information Springfield, Virginia 22151 - Price 56.00 I - TABLE OF CONTENTS Page SUMMA=. 1 INTRODUCTION. i SECTION I. CHARACTERISTICS OF THE MOON. i . 3 Chapter 1. The Moon’s .History, by Ernst Stuhlinger. 5 Chapter 2. Physical Characteristics of the Lunar Surface, by John Bensko . 39 Chapter 3. The’ Lunar Atmosphere, by Spencer G. Frary . , 55 Chapter 4. Energetic Radiation Environment of the Moon, by Martin 0. Burrell . 65 Chapter 5. The Lunar Thermal Environment , . 9i The Thermal Model of the Moon, by Gerhard B. Heller . 91 p Thermal Properties of the Moon as a Conductor of Heat,byBillyP. Jones.. 121 Infrared Methods of Measuring the Moon’s Temperature, by Charles D. Cochran. 135 SECTION II. EXPLORATION OF THE MOON . .I59 Chapter I. A Lunar Scientific Mission, by Daniel Payne Hale. 161 Chapter 2. Some Suggested Landing Sites for Exploration of the Moon, by Daniel Payne Hale. 177 Chapter 3. Environmental Control for Early Lunar Missions, by ‘Herman P. Gierow and James A. Downey, III . , . .2i I Chapter 4.
    [Show full text]
  • Arxiv:2008.01837V1 [Astro-Ph.EP] 4 Aug 2020 Sunlight Is Transmitted to the Lunar Surface at Altitudes Where It Passes Through the O3 Layer Rather Than Above It
    Draft version August 6, 2020 Typeset using LATEX preprint style in AASTeX62 The Hubble Space Telescope's near-UV and optical transmission spectrum of Earth as an exoplanet Allison Youngblood,1, 2 Giada N. Arney,2, 3, 4 Antonio Garc´ıa Munoz,~ 5 John T. Stocke,6 Kevin France,1, 6 and Aki Roberge2 1Laboratory for Atmospheric and Space Physics, 1234 Innovation Dr, Boulder, CO 80303, USA 2NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 3NASA NExSS Virtual Planetary Laboratory, P.O. Box 351580, Seattle, WA 98195, USA 4Sellers Exoplanet Environments Collaboration, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 5Zentrum f¨urAstronomie und Astrophysik, Technische Universit¨atBerlin, Hardenbergstrasse 36, D-10623, Berlin, Germany 6Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, UCB 389, Boulder, CO 80309, USA ABSTRACT We observed the 2019 January total lunar eclipse with the Hubble Space Telescope's STIS spectrograph to obtain the first near-UV (1700-3200 A)˚ observation of Earth as a transiting exoplanet. The observatories and instruments that will be able to perform transmission spectroscopy of exo-Earths are beginning to be planned, and characteriz- ing the transmission spectrum of Earth is vital to ensuring that key spectral features (e.g., ozone, or O3) are appropriately captured in mission concept studies. O3 is photo- chemically produced from O2, a product of the dominant metabolism on Earth today, and it will be sought in future observations as critical evidence for life on exoplanets. Ground-based observations of lunar eclipses have provided the Earth's transmission spectrum at optical and near-IR wavelengths, but the strongest O3 signatures are in the near-UV.
    [Show full text]
  • Geophysical Abstracts 186 July-September 1961
    Geophysical Abstracts 186 July-September 1961 By JAMES W. CLARKE, DOROTHY B. VITALIANO, VIRGINIA S. NEUSCHEL, and others GEOLOGICAL SURVEY BULLETIN 1146-C Abstracts of current literature pertaining to the physics of the solid earth and to geophysical exploration UNITED STATES GOVERNMENT PRINTING OFFICE, WASHINGTON : 1961 UNITED STATES DEPARTMENT OF THE INTERIOR STEWART L. UDALL, Secretary GEOLOGICAL SURVEY Thomas B. Nolan, Director For sale by the Superintendent of Documents, U.S. Government Printtna Office, Washintlton 25, D.C. Price 40 cents (sintUe copy). Subacription price: $1.75 a year; 50 cents additional for foreilln mattin!l. Use of funds for printing this publication has been approved by the Director of the Bureau of the Budget (June 23, 1960). CONTENTS Page Introduction --------------------------------------------------- 351 Extent of coverage ------------------------------------------ 351 List of journals--------------------------------------------- 351 Form of citation-------------------------------------------- 353 Abstracters ------------------------------------------------ 353 Age determinations -------------------------------------------- 353 Cosmogony---------------------------------------------------- 366 Earth currents ------------------------------------------------ 385 Earthquakes and earthquake waves------------------------------- 387 Earth tides and related phenomena------------------------------- 413 Elasticity ----------------------------------------------------- 416 Electrical exploration------------------------------------------
    [Show full text]
  • Ultraviolet Spectral Radiant Energy Reflected from the Moon
    Journal of Research of the National Bureau of Standards Vol. 5 1, No, 2, August 1953 Research Paper 2434 Ultraviolet Spectral Radiant Energy Reflected From the Moon Ralph Stair and Russell Johnston R esults are given of some measurements on t he ultraviolet and short-wavelengtll visi,b le s ectral radiant energy reflected from t he surface of the full moon, made from October to ~ rnber 1952 at Washington D , C. Although t he reflected lunar spectrum co ntarn s a ll t h~eF raunh o re r' bands as found in ?irect sunlight .with approximately t he s ame r~ e l aL r ve intensities in t he visible spectrum, In tense ab so rp t r ~ n occur's for some. of the ult raviolet wavelengths. Selective absorption for wavelengths III the spe?tT1!-l regrons of 380 to ~9 0 millimicrons and less t han 360 millimicrons indicates t he pOSSIbility of a lunar re flectrn g surface s imi la r to t hat of powdered glassy silicates. 1. Introduction range incident on th e ~oon . l'!le co ll e~ti~m <?f a . thin layer of fine meteOrIC matenal contammg Iron Man has long speculated abo:ut the I1?-0on- lts and other dark substances may be expected also to orio'in its surface features, and Its path III space. darken the lunar surface. This interest has stimulated the search for facts The study of the moon through m easurem ent of Its regarding the exact nature and origin of the surface effect upon r efl ected sunlight may ~e .appro~ ch ed panorama visible through the telescope.
    [Show full text]
  • Manned Spacecraft Center Houston, Texas
    If" S r, 3ii i uiIF yy.ij. ULULUUiutu. uufi NATIONAL AERONAUTICS AND SPACE ADMINISTRATION EARTH RESOURCES SURVEY PROGRAM TECHNICAL LETTER NASA-95 A SURVEY OF LUNAR GEOLOGY By Jerald J. Cook Willow Run Laboratories Institute of Science and Technology Ann Arbor, Michigan November 1967 Prepared by the Geological Survey for the National Aeronautics and Space Administration (NASA) under NASA Contract No. R-146-09-020-006 MANNED SPACECRAFT CENTER HOUSTON, TEXAS -753,77 UNITED STATES Interagency Report DEPARTMENT OF THE INTERIOR NASA-95 GEOLOGICAL SURVEY November 1967 WASHINGTON. D.C. 20242 Colonel Michael Ahmajan Acting Chief, Earth Resources Discipline Surveys Office of Space Science and Applications Code SAR - NASA Headquarters RETURN TO: Washington, D.C. 20546 NMD RESEARCH REFERENCE COLLECTION USGS NATIONAL CENTER, MS-521 Dear Colonel Ahmajan: RESIGN, VA 22092 Transmitted herewith is one copy of: INTERAGENCY REPORT NASA-95 A SURVEY OF LUNAR GEOLOGY* by Jerald J. Cook** The U.S. Geological Survey has released this report in open files. Copies are available for consultation in the Geological Survey Libraries, 1033 GSA Building, Washington, D.C. 20242; Building 25, Federal Center, Denver, Colorado 80225; and 345 Middlefield Road, Menlo Park, California 94025. Sincerely yours, William A. Fischer Research Coordinator Earth Orbiter Program *Work performed under NASA Contract No. R-146-09-020-006 **Willow Run Laboratories of the Institute of Science and Technology, University of Michigan, Ann Arbor, Michigan UNITED STATES DEPARTMENT OF THE INTERIOR GEOLOGICAL SURVEY INTERAGENCY REPORT NASA-95 SURVEY OF LUNAR GEOLOGY* by Jerald J. Cook** November 1967 The work reported herein was conducted by the Willow Run Laboratories of the Institute of Science and Technology, University-of Michigan on behalf of the U.S.
    [Show full text]