Final Report of the Advancing Science Of
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
A Wunda-Full World? Carbon Dioxide Ice Deposits on Umbriel and Other Uranian Moons
Icarus 290 (2017) 1–13 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus A Wunda-full world? Carbon dioxide ice deposits on Umbriel and other Uranian moons ∗ Michael M. Sori , Jonathan Bapst, Ali M. Bramson, Shane Byrne, Margaret E. Landis Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA a r t i c l e i n f o a b s t r a c t Article history: Carbon dioxide has been detected on the trailing hemispheres of several Uranian satellites, but the exact Received 22 June 2016 nature and distribution of the molecules remain unknown. One such satellite, Umbriel, has a prominent Revised 28 January 2017 high albedo annulus-shaped feature within the 131-km-diameter impact crater Wunda. We hypothesize Accepted 28 February 2017 that this feature is a solid deposit of CO ice. We combine thermal and ballistic transport modeling to Available online 2 March 2017 2 study the evolution of CO 2 molecules on the surface of Umbriel, a high-obliquity ( ∼98 °) body. Consid- ering processes such as sublimation and Jeans escape, we find that CO 2 ice migrates to low latitudes on geologically short (100s–1000 s of years) timescales. Crater morphology and location create a local cold trap inside Wunda, and the slopes of crater walls and a central peak explain the deposit’s annular shape. The high albedo and thermal inertia of CO 2 ice relative to regolith allows deposits 15-m-thick or greater to be stable over the age of the solar system. -
Copyrighted Material
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 -
New Candidate Pits and Caves at High Latitudes on the Near Side of the Moon
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 2733.pdf NEW CANDIDATE PITS AND CAVES AT HIGH LATITUDES ON THE NEAR SIDE OF THE MOON. 1,2 1,3,4 1 2 Wynnie Avent II and Pascal Lee , S ETI Institute, Mountain View, VA, USA, V irginia Polytechnic Institute 3 4 and State University Blacksburg, VA, USA. M ars Institute, N ASA Ames Research Center. Summary: 35 new candidate pits are identified in Anaxagoras and Philolaus, two high-latitude impact structures on the near side of the Moon. Introduction: Since the discovery in 2009 of the Marius Hills Pit (Haruyama et al. 2009), a.k.a. the “Haruyama Cavern”, over 300 hundred pits have been identified on the Moon (Wagner & Robinson 2014, Robinson & Wagner 2018). Lunar pits are small (10 to 150 m across), steep-walled, negative relief features (topographic depressions), surrounded by funnel-shaped outer slopes and, unlike impact craters, no raised rim. They are interpreted as collapse features resulting from the fall of the roof of shallow (a few Figure 1: Location of studied craters (Polar meters deep) subsurface voids, generally lava cavities. projection). Although pits on the Moon are found in mare basalt, impact melt deposits, and highland terrain of the >300 Methods: Like previous studies searching for pits pits known, all but 16 are in impact melts (Robinson & (Wagner & Robinson 2014, Robinson & Wagner 2018, Wagner 2018). Many pits are likely lava tube skylights, Lee 2018a,b,c), we used imaging data collected by the providing access to underground networks of NASA Lunar Reconnaissance Orbiter (LRO) Narrow tunnel-shaped caves, including possibly complex Angle Camera (NAC). -
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. -
Evidence for Thermal-Stress-Induced Rockfalls on Mars Impact Crater Slopes
Icarus 342 (2020) 113503 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Evidence for thermal-stress-induced rockfalls on Mars impact crater slopes P.-A. Tesson a,b,*, S.J. Conway b, N. Mangold b, J. Ciazela a, S.R. Lewis c, D. M�ege a a Space Research Centre, Polish Academy of Science, Wrocław, Poland b Laboratoire de Plan�etologie et G�eodynamique UMR 6112, CNRS, Nantes, France c School of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK ARTICLE INFO ABSTRACT Keywords: Here we study rocks falling from exposed outcrops of bedrock, which have left tracks on the slope over which Mars, surface they have bounced and/or rolled, in fresh impact craters (1–10 km in diameter) on Mars. The presence of these Thermal stress tracks shows that these rocks have fallen relatively recently because aeolian processes are known to infill Ices topographic lows over time. Mapping of rockfall tracks indicate trends in frequency with orientation, which in Solar radiation � � turn depend on the latitudinal position of the crater. Craters in the equatorial belt (between 15 N and 15 S) Weathering exhibit higher frequencies of rockfall on their north-south oriented slopes compared to their east-west ones. � Craters >15 N/S have notably higher frequencies on their equator-facing slopes as opposed to the other ori entations. We computed solar radiation on the surface of crater slopes to compare insolation patterns with the spatial distribution of rockfalls, and found statistically significant correlations between maximum diurnal inso lation and rockfall frequency. -
Apollo Program 1 Apollo Program
Apollo program 1 Apollo program The Apollo program was the third human spaceflight program carried out by the National Aeronautics and Space Administration (NASA), the United States' civilian space agency. First conceived during the Presidency of Dwight D. Eisenhower as a three-man spacecraft to follow the one-man Project Mercury which put the first Americans in space, Apollo was later dedicated to President John F. Kennedy's national goal of "landing a man on the Moon and returning him safely to the Earth" by the end of the 1960s, which he proposed in a May 25, 1961 address to Congress. Project Mercury was followed by the two-man Project Gemini (1962–66). The first manned flight of Apollo was in 1968 and it succeeded in landing the first humans on Earth's Moon from 1969 through 1972. Kennedy's goal was accomplished on the Apollo 11 mission when astronauts Neil Armstrong and Buzz Aldrin landed their Lunar Module (LM) on the Moon on July 20, 1969 and walked on its surface while Michael Collins remained in lunar orbit in the command spacecraft, and all three landed safely on Earth on July 24. Five subsequent Apollo missions also landed astronauts on the Moon, the last in December 1972. In these six spaceflights, 12 men walked on the Moon. Apollo ran from 1961 to 1972, and was supported by the two-man Gemini program which ran concurrently with it from 1962 to 1966. Gemini missions developed some of the space travel techniques that were necessary for the success of the Apollo missions. -
2021 Transpacific Yacht Race Event Program
TRANSPACTHE FIFTY-FIRST RACE FROM LOS ANGELES 2021 TO HONOLULU 2 0 21 JULY 13-30, 2021 Comanche: © Sharon Green / Ultimate Sailing COMANCHE Taxi Dancer: © Ronnie Simpson / Ultimate Sailing • Hamachi: © Team Hamachi HAMACHI 2019 FIRST TO FINISH Official race guide - $5.00 2019 OVERALL CORRECTED TIME WINNER P: 808.845.6465 [email protected] F: 808.841.6610 OFFICIAL HANDBOOK OF THE 51ST TRANSPACIFIC YACHT RACE The Transpac 2021 Official Race Handbook is published for the Honolulu Committee of the Transpacific Yacht Club by Roth Communications, 2040 Alewa Drive, Honolulu, HI 96817 USA (808) 595-4124 [email protected] Publisher .............................................Michael J. Roth Roth Communications Editor .............................................. Ray Pendleton, Kim Ickler Contributing Writers .................... Dobbs Davis, Stan Honey, Ray Pendleton Contributing Photographers ...... Sharon Green/ultimatesailingcom, Ronnie Simpson/ultimatesailing.com, Todd Rasmussen, Betsy Crowfoot Senescu/ultimatesailing.com, Walter Cooper/ ultimatesailing.com, Lauren Easley - Leialoha Creative, Joyce Riley, Geri Conser, Emma Deardorff, Rachel Rosales, Phil Uhl, David Livingston, Pam Davis, Brian Farr Designer ........................................ Leslie Johnson Design On the Cover: CONTENTS Taxi Dancer R/P 70 Yabsley/Compton 2019 1st Div. 2 Sleds ET: 8:06:43:22 CT: 08:23:09:26 Schedule of Events . 3 Photo: Ronnie Simpson / ultimatesailing.com Welcome from the Governor of Hawaii . 8 Inset left: Welcome from the Mayor of Honolulu . 9 Comanche Verdier/VPLP 100 Jim Cooney & Samantha Grant Welcome from the Mayor of Long Beach . 9 2019 Barndoor Winner - First to Finish Overall: ET: 5:11:14:05 Welcome from the Transpacific Yacht Club Commodore . 10 Photo: Sharon Green / ultimatesailingcom Welcome from the Honolulu Committee Chair . 10 Inset right: Welcome from the Sponsoring Yacht Clubs . -
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, -
Apollo 12 Photography Index
%uem%xed_ uo!:q.oe_ s1:s._l"e,d_e_em'I flxos'p_zedns O_q _/ " uo,re_ "O X_ pea-eden{ Z 0 (D I I 696L R_K_D._(I _ m,_ -4 0", _z 0', l',,o ._ rT1 0 X mm9t _ m_o& ]G[GNI XHdV_OOZOHd Z L 0T'I0_V 0 0 11_IdVdONI_OM T_OINHDZZ L6L_-6 GYM J_OV}KJ_IO0VSVN 0 C O_i_lOd-VJD_IfO1_d 0 _ •'_ i wO _U -4 -_" _ 0 _4 _O-69-gM& "oN GSVH/O_q / .-, Z9946T-_D-VSVN FOREWORD This working paper presents the screening results of Apollo 12, 70mmand 16mmphotography. Photographic frame descriptions, along with ground coverage footprints of the Apollo 12 Mission are inaluded within, by Appendix. This report was prepared by Lockheed Electronics Company,Houston Aerospace Systems Division, under Contract NAS9-5191 in response to Job Order 62-094 Action Document094.24-10, "Apollo 12 Screening IndeX', issued by the Mapping Sciences Laboratory, MannedSpacecraft Center, Houston, Texas. Acknowledgement is made to those membersof the Mapping Sciences Department, Image Analysis Section, who contributed to the results of this documentation. Messrs. H. Almond, G. Baron, F. Beatty, W. Daley, J. Disler, C. Dole, I. Duggan, D. Hixon, T. Johnson, A. Kryszewski, R. Pinter, F. Solomon, and S. Topiwalla. Acknowledgementis also made to R. Kassey and E. Mager of Raytheon Antometric Company ! I ii TABLE OF CONTENTS Section Forward ii I. Introduction I II. Procedures 1 III. Discussion 2 IV. Conclusions 3 V. Recommendations 3 VI. Appendix - Magazine Summary and Index 70mm Magazine Q II II R ii It S II II T II I! U II t! V tl It .X ,, ,, y II tl Z I! If EE S0-158 Experiment AA, BB, CC, & DD 16mm Magazines A through P VII. -
Water on the Moon, III. Volatiles & Activity
Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere). -
Determining the Structural Stability of Lunar Lava Tubes
46th Lunar and Planetary Science Conference (2015) 2174.pdf DETERMINING THE STRUCTURAL STABILITY OF LUNAR LAVA TUBES. D. M. Blair1*, L. Chappaz2, R. Sood2, C. Milbury1, H. J. Melosh1, K. C. Howell2, and A. M. Freed1. 1,* Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA, [email protected]; 2School of Aeronautics and Astronautics, Purdue University, West Lafayette, IN, USA. Introduction: Recent in-depth analysis of lunar wider lava tube or a thinner roof, but do not quantify gravity data from the Gravity Recovery And Interior what difference an arched roof would make. Laboratory (GRAIL) spacecraft has suggested the In caves on Earth that occur in bedded rock, failure possibility of lava tubes on the Moon with diameters in of the cave’s roof tends to occur one bed at a time, excess of 1 km [1, 2]. Could such features be progressing upwards [9]. This means that the structurally stable? What is the theoretical maximum mechanical “roof thickness” of a lava tube should be size of a lunar lava tube? Here we attempt to address considered to be the thickness of the flows that form those questions and improve on prior estimates of the the roof and not the total depth at which the tube is same by using modern numerical modeling techniques. buried. Lava flows thicknesses on the moon vary over Background: The presence of sublunarean voids a broad range, from 1–14 m in the skylights in Mare has recently been confirmed via the observation of Tranquilitatis and elsewhere [5] to ~80–600 m in "skylights" in several lunar maria [3, 4, 5]. -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei