Planetary Nomenclature: Information and Guidelines for Geologic Mappers
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Planetary Nomenclature: an Overview and Update
3rd Planetary Data Workshop 2017 (LPI Contrib. No. 1986) 7119.pdf PLANETARY NOMENCLATURE: AN OVERVIEW AND UPDATE. T. Gaither1, R. K. Hayward1, J. Blue1, L. Gaddis1, R. Schulz2, K. Aksnes3, G. Burba4, G. Consolmagno5, R. M. C. Lopes6, P. Masson7, W. Sheehan8, B.A. Smith9, G. Williams10, C. Wood11, 1USGS Astrogeology Science Center, Flagstaff, Ar- izona ([email protected]); 2ESA Scientific Support Office, Noordwijk, The Netherlands; 3Institute for Theoretical Astrophysics, Oslo, Norway; 4Vernadsky Institute, Moscow, Russia; 5Specola Vaticana, Vati- can City State; 6Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California; 7Uni- versite de Paris-Sud, Orsay, France; 8Lowell Observatory, Flagstaff, Arizona; 9Santa Fe, New Mexico; 10Minor Planet Center, Cambridge, Massachusetts; 11Planetary Science Institute, Tucson, Arizona. Introduction: The task of naming planetary Asteroids surface features, rings, and natural satellites is Ceres 113 managed by the International Astronomical Un- Dactyl 2 ion’s (IAU) Working Group for Planetary System Eros 41 Nomenclature (WGPSN). The members of the Gaspra 34 WGPSN and its task groups have worked since the Ida 25 early 1970s to provide a clear, unambiguous sys- Itokawa 17 tem of planetary nomenclature that represents cul- Lutetia 37 tures and countries from all regions of Earth. Mathilde 23 WGPSN members include Rita Schulz (chair) and Steins 24 9 other members representing countries around the Vesta 106 globe (see author list). In 2013, Blue et al. [1] pre- Jupiter sented an overview of planetary nomenclature, and Amalthea 4 in 2016 Hayward et al. [2] provided an update to Thebe 1 this overview. Given the extensive planetary ex- Io 224 ploration and research that has taken place since Europa 111 2013, it is time to update the community on the sta- Ganymede 195 tus of planetary nomenclature, the purpose and Callisto 153 rules, the process for submitting name requests, and the IAU approval process. -
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. -
Mapping of Inner and Outer Celestial Bodies Using New Global and Local Topographic Data Derived from Photogrammetric Image Processing
The International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences, Volume XLI-B4, 2016 XXIII ISPRS Congress, 12–19 July 2016, Prague, Czech Republic Mapping of inner and outer celestial bodies using new global and local topographic data derived from photogrammetric image processing I.P. Karachevtsevaa*, A.A. Kokhanova, J.F. Rodionovaa,b, A.Yu. Zharkovaa,, M.S. Lazarevaa aMoscow State University of Geodesy and Cartography (MIIGAiK), MIIGAiK Extraterrestrial laboratory (MExLab), 105064. Gorokhovsky per., Moscow, Russia [email protected] bSternberg State Astronomical Institute, 1198993, Moscow, Russia Commission IV, WG IV/8 KEY WORDS: Planetary cartography, DEM, geomorphology study, Phobos, the Moon, Mercury, Ganymede and Enceladus ABSTRACT: New estimation of fundamental geodetic parameters and global and local topography of planets and satellites provide basic coordinate systems for mapping as well as opportunities for studies of processes on their surfaces. The main targets of our study are Europa, Ganymede, Calisto and Io (satellites of Jupiter), Enceladus (a satellite of Saturn), terrestrial planetary bodies, including Mercury, the Moon and Phobos, one of the Martian satellites. In particular, based on new global shape models derived from three-dimensional control point networks and processing of high-resolution stereo images, we have carried out studies of topography and morphology. As a visual representation of the results, various planetary maps with different scale and thematic direction were created. For example, for Phobos we have produced a new atlas with 43 maps, as well as various wall maps (different from the maps in the atlas by their format and design): basemap, topography and geomorphological maps. In addition, we compiled geomorphologic maps of Ganymede on local level, and a global hypsometric Enceladus map. -
Triton: Topography and Geology of a Probable Ocean World with Comparison to Pluto and Charon
remote sensing Article Triton: Topography and Geology of a Probable Ocean World with Comparison to Pluto and Charon Paul M. Schenk 1,* , Chloe B. Beddingfield 2,3, Tanguy Bertrand 3, Carver Bierson 4 , Ross Beyer 2,3, Veronica J. Bray 5, Dale Cruikshank 3 , William M. Grundy 6, Candice Hansen 7, Jason Hofgartner 8 , Emily Martin 9, William B. McKinnon 10, Jeffrey M. Moore 3, Stuart Robbins 11 , Kirby D. Runyon 12 , Kelsi N. Singer 11 , John Spencer 11, S. Alan Stern 11 and Ted Stryk 13 1 Lunar and Planetary Institute, Houston, TX 77058, USA 2 SETI Institute, Palo Alto, CA 94020, USA; chloe.b.beddingfi[email protected] (C.B.B.); [email protected] (R.B.) 3 NASA Ames Research Center, Moffett Field, CA 94035, USA; [email protected] (T.B.); [email protected] (D.C.); [email protected] (J.M.M.) 4 School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85202, USA; [email protected] 5 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85641, USA; [email protected] 6 Lowell Observatory, Flagstaff, AZ 86001, USA; [email protected] 7 Planetary Science Institute, Tucson, AZ 85704, USA; [email protected] 8 Jet Propulsion Laboratory, Pasadena, CA 91001, USA; [email protected] 9 National Air & Space Museum, Washington, DC 20001, USA; [email protected] 10 Department of Earth and Planetary Sciences, Washington University in Saint Louis, Saint Louis, MO 63101, USA; [email protected] 11 Southwest Research Institute, Boulder, CO 80301, USA; [email protected] (S.R.); [email protected] (K.N.S.); [email protected] (J.S.); [email protected] (S.A.S.) Citation: Schenk, P.M.; Beddingfield, 12 Johns Hopkins Applied Physics Laboratory, Laurel, MD 20707, USA; [email protected] 13 C.B.; Bertrand, T.; Bierson, C.; Beyer, Humanities Division, Roane State Community College, Harriman, TN 37748, USA; [email protected] R.; Bray, V.J.; Cruikshank, D.; Grundy, * Correspondence: [email protected] W.M.; Hansen, C.; Hofgartner, J.; et al. -
Mercury Redux
FEATURE Mercury redux In January 2008, 33 years after Mariner 10 fl ew past the solar system’s innermost planet, MESSENGER crossed Mercury’s magnetosphere. Ancient volcanoes, contractional faults, and a rich soup of exospheric ions give clues to Mercury’s structure and dynamical evolution. Th e Mercury fl yby of the MESSENGER two have not been ruled out, but for those (Mercury surface, space environment, mechanisms shorter-wavelength magnetic geochemistry and ranging) probe was the features would be expected, which were not fi rst of three braking manoeuvres for the observed during the MESSENGER fl yby1. spacecraft , in preparation for its insertion Recent libration observations that require into a polar orbit in 2011. Th e probe a partially molten core11, and the limited achieved the closest approach (201 km) of contraction of Mercury, which implies a Mercury’s surface yet, and took a variety largely molten core, favour a convective of measurements in the magnetosphere, dynamo origin for Mercury’s magnetic fi eld. exosphere and on Mercury’s surface. Some Although Mercury’s magnetosphere of the fi rst results of the MESSENGER looks like a miniature version of Earth’s, mission1–6 reveal Mercury as a planet with Mercury’s relatively weak magnetic richly interconnected dynamics, from fi eld implies that its dynamo must work the dynamo in its molten outer core, a diff erently from that of the Earth. Th e crust and surface with great lobate faults geodynamo, which gives the Earth its and relatively young volcanoes, to a strong magnetic fi eld, is thought to operate magnetosphere that interacts with the core in a magnetostrophic regime in which the dynamo and the interplanetary solar wind. -
Geologic Map of the Ganiki Planitia Quadrangle (V–14), Venus Eric B
Claremont Colleges Scholarship @ Claremont Pomona Faculty Publications and Research Pomona Faculty Scholarship 1-1-2011 Geologic Map of the Ganiki Planitia Quadrangle (V–14), Venus Eric B. Grosfils Pomona College Sylvan M. Long Elizabeth M. Venechuk Debra M. Hurwitz Joseph W. Richards See next page for additional authors Recommended Citation Grosfils, E.B., Long, S.M., Venechuk, E.M., Hurwitz, D.M., Richards, J.W., Kastl, Brian, Drury, D.E., and Hardin, Johanna, 2011, Geologic map of the Ganiki Planitia quadrangle (V-14), Venus: U.S. Geological Survey Scientific nI vestigations Map 3121. This Report is brought to you for free and open access by the Pomona Faculty Scholarship at Scholarship @ Claremont. It has been accepted for inclusion in Pomona Faculty Publications and Research by an authorized administrator of Scholarship @ Claremont. For more information, please contact [email protected]. Authors Eric B. Grosfils, Sylvan M. Long, Elizabeth M. Venechuk, Debra M. Hurwitz, Joseph W. Richards, Brian Kastl, Dorothy E. Drury, and Johanna S. Hardin This report is available at Scholarship @ Claremont: http://scholarship.claremont.edu/pomona_fac_pub/303 Prepared for the National Aeronautics and Space Administration Geologic Map of the Ganiki Planitia Quadrangle (V–14), Venus By Eric B. Grosfils, Sylvan M. Long, Elizabeth M. Venechuk, Debra M. Hurwitz, Joseph W. Richards, Brian Kastl, Dorothy E. Drury, and Johanna Hardin Pamphlet to accompany Scientific Investigations Map 3121 75° 75° V–1 V–3 V–6 50° 50° V–4 V–5 V–11 V–16 V–12 V–15 V–13 V–14 25° 25° V–23 V–28 V–24 V–27 V–25 V–26 90° 120° 150° 180° 210° 240° 270° 0° 0° V–37 V–38 V–36 V–39 V–35 V–40 –25° –25° V–49 V–50 V–48 V–51 V–47 V–52 V–58 V–59 –50° –50° V–57 V–60 2011 V–62 –75° –75° U.S. -
GEOLOGIC MAPS of the OLYMPUS MONS REGION of MARS by Elliot C. Morris and Kenneth L. Tanaka
U.S. DEPARTMENT OF THE INTERIOR U.S. GEOLOGICAL SURVEY GEOLOGIC MAPS OF THE OLYMPUS MONS REGION OF MARS By Elliot C. Morris and Kenneth L. Tanaka Prepared for the NATIONAL AERONAUTICS AND SPACE ADMINISTRATION ..... t\:) a 0 a0 0 0 )> z 0 ..... ..... MISCELLANEOUS INVESTIGATIONS SERIES a 0 Published by the U.S. Geological Survey, 1994 a0 0 0 3: ~ U.S. DEPARTMENT OF THE INTERIOR TO ACCOMPANY MAP I-2327 U.S. GEOLOGICAL SURVEY GEOLOGIC MAPS OF THE OLYMPUS MONS REGION OF MARS By Elliot C. Morris and Kenneth L. Tanaka INTRODUCTION measurements of relief valuable in determining such factors as Olympus Mons is one of the broadest volcanoes and volcano volume, structural offsets, and lava-flow rheology. certainly the tallest in the Solar System. It has been extensively Except for the difference in extent of the areas mapped, the described and analyzed in scientific publications and frequently topographic information, the cartographic control (latitudes noted in the popular and nontechnical literature of Mars. and longitudes of features may differ by as much as a few tenths However, the first name given to the feature-Nix Olympica of a degree), and the greater detail permitted by the larger scale (Schiaparelli, 1879)-was based on its albedo, not its size, base, the two maps are virtually the same. A comparison of our because early telescopic observations of Mars revealed only map units with those of other Viking-based maps is given in albedo features and not topography (lnge and others, 1971). table 1. After Mariner 9 images acquired in 1971 showed that this Unravellng the geology of the Olympus Mons region is not albedo feature coincides with a giant shield volcano (McCauley limited to a simple exercise in stratigraphy. -
Mysterious Mercury Bepicolumbo Heads for the World of Ice and Fire
A Digital Supplement to Astronomy Insights Astronomy Magazine © 2018 Kalmbach Media Mysterious Mercury BepiColumbo Heads for the World of Ice and Fire Dcember 2018 • Astronomy.com Voyage to a world Color explodes from Mercury’s surface in this enhanced-color mosaic taken through several filters. The yellow and orange hues signify relatively young plains likely formed when fluid lavas erupted from volcanoes. Medium- and dark-blue regions are older terrain, while the light-blue and white streaks represent fresh material excavated from relatively recent impacts. ALL IMAGES, UNLESS OTHERWISE NOTED: NASA/JHUAPL/CIW 2 ASTRONOMY INSIGHTS • DECEMBER 2018 A world of both fire and ice, Mercury excites and confounds scientists. The BepiColombo probe aims to make sense of this mysterious world. by Ben Evans of extremesWWW.ASTRONOMY.COM 3 Mercury is a land of contrasts. The solar system’s smallest planet boasts the largest core relative to its size. Temperatures at noon can soar as high as 800 degrees Fahrenheit (425 degrees Celsius) — hot enough to melt lead — but dip as low as –290 F (–180 C) before dawn. Mercury resides nearest the Sun, and it has the most eccentric orbit. At its closest, the planet lies only 29 mil- lion miles (46 million kilometers) from the Sun — less than one-third Earth’s distance — but swings out as far as 43 million miles (70 million km). Its rapid movement across our sky earned it a reputation among ancient skywatchers as the fleet-footed messenger of the gods: Italian scientist Giuseppe “Bepi” Colombo helped develop a technique for sending a space Hermes to the Greeks and Mercury to the Romans. -
Compressional Tectonism on Mars
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 98, NO. E9, PAGES 17,049-17,060, SEPTEMBER 25, 1993 Compressional Tectonism on Mars THOMAS R. WATTERS Centerfor Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington,D.C. Contractional features on Mars were identified on the basis of photogeologic evidence of crustal shortening and comparison with terrestrial and planetary analogs. Three classes of structures, wrinkle ridges. lobate scarps and high-relief ridges. were mapped and their spatial and temporal distribution assessed. Wrinkle ridges account for over 80% of the total cumulative length of the mapped contractional features and occur in smooth plains material interpreted to be volcanic in origin. Lobate scarps, not wrinkle ridges, are the dominant contractional feature in Martian highland material. The pattern of contractional features in the western hemisphere reflects the hemispheric-scale iduence of the Tharsis rise. Although no comparable hemispheric- scale pattern is observed in the eastern hemisphere, prominent regional-scale patterns exist, the most notable of which occurs in Hesperia Planum. Contractional features that locally parallel the trend of the cmstal dichotomy boundary in the eastern hemisphere suggest the influence of stresses related to the evolution of the dichotomy. Compressional deformation apparently peaked during the Early Hesperia, if the tectonic features are roughly the same age as the units in which they occur. This peak in compressional deformation corresponds with Early Hesperian volcanic resurfacing of a large portion of the planet. Thermal history models for Mars, based on an initially hot planet, are inconsistent with estimates of the timing of peak compressional tectonism and the rate of volcanism. -
Nomenclature for Lunar Features at the Chang'e-3 Landing Site
Acta Geochim (2017) 36(2):213–223 DOI 10.1007/s11631-017-0159-1 ORIGINAL ARTICLE Nomenclature for lunar features at the Chang’e-3 landing site Zhoubin Zhang1,2 · Chunlai Li1,2,3 · Wei Zuo1,2,3 · Xingguo Zeng1,2 Received: 22 December 2016 / Revised: 15 February 2017 / Accepted: 9 April 2017 / Published online: 27 April 2017 © Science Press, Institute of Geochemistry, CAS and Springer-Verlag Berlin Heidelberg 2017 Abstract Nomenclatures for lunar features always published after some necessary approval procedures by the accompany the progresses of human lunar exploration, International Astronomical Union. which has an important dual meaning in culture and sci- ence. The naming of lunar features not only can Keywords Moon · Chang’e-3 · Landing site · Lunar commemorate the outstanding contributions of academics, feature nomenclature masters in various fields, and popularize the traditional cultures of ethnic groups all over the world, but also have a critical function of providing accurate indicative informa- 1 Introduction tion on features with special morphology, origin, nature and scientific value. However, nomenclature for features at Planetary nomenclature, like terrestrial nomenclature, is the Chang’e-3 landing site, which has a more arbitrary used to uniquely identify a feature on the surface of a form without many constrains posed by a uniformed sys- planet or satellite so that the feature can be easily located, tem, is unlike the features for other morphological units. described, and discussed. Nomenclature for lunar features This paper originated from the actual needs for the originated in the seventeenth century, as early scientists in description of scientific exploration activities, interpreta- that era used telescopes to observe the lunar surface, named tion of scientific research and dissemination of scientific the remarkable features on the lunar surface according to results. -
Mars Activities
MARS ACTIVITIES Teacher Resources and Classroom Activities Mars Education Program Jet Propulsion Laboratory Arizona State University Mars Missions Information and Updates Mission Information Available at Jet Propulsion Laboratory Mars Exploration Home Page http://mars.jpl.nasa.gov More Educational Activities Available at Jet Propulsion Laboratory Mars Education & Public Outreach Program http://mars.jpl.nasa.gov/classroom or Arizona State University Mars K-12 Education Program http://tes.asu.edu/neweducation.html Table of Contents 1. Earth, Moon, Mars Balloons 1 2. Rover Races 4 3. Areology - The Study of Mars 11 4. Strange New Planet 16 5. Lava Layering 24 6. Searching for Life on Mars 33 7. Mars Critters 42 8. Exploring Crustal Material from a Mystery Planet 46 - Graph Paper 48 9. Edible Mars Rover 49 - Mars Pathfinder Rover 51 10. Edible Mars Spacecraft 52 - Mars Global Surveyor 54 - Mars Pathfinder 55 - Mars Pathfinder Rover 56 11. Mars Meteorites’ Fingerprints 57 12. Introduction to Creating a Mission Plan 65 13. Out of Sight: Remote Vehicle Activity 66 - Mars Rover Websites 69 15. Probing Below the Surface of Mars 74 16. Good Vibrations 85 17. The Mathematics of Mars 90 - “I Have…Who Has?” Cards 93 18. Mars Bingo 100 19. Mud Splat Craters 112 20. Solar System Beads Distance Activity 115 21. Alka-Seltzer Rockets 118 22. Soda Straw Rockets 122 23. Mars Pathfinder: Two-Dimensional Model 126 24. Mars Pathfinder: Egg Drop and Landing 127 25. Cool Internet Sites 128 Earth, Moon, Mars Balloons 1 Introduction: How big is the Moon; how far is it relative to Earth? Earth science and astronomy books depict a moon that is much closer and much larger than in reality. -
Features Named After 07/15/2015) and the 2018 IAU GA (Features Named Before 01/24/2018)
The following is a list of names of features that were approved between the 2015 Report to the IAU GA (features named after 07/15/2015) and the 2018 IAU GA (features named before 01/24/2018). Mercury (31) Craters (20) Akutagawa Ryunosuke; Japanese writer (1892-1927). Anguissola SofonisBa; Italian painter (1532-1625) Anyte Anyte of Tegea, Greek poet (early 3rd centrury BC). Bagryana Elisaveta; Bulgarian poet (1893-1991). Baranauskas Antanas; Lithuanian poet (1835-1902). Boznańska Olga; Polish painter (1865-1940). Brooks Gwendolyn; American poet and novelist (1917-2000). Burke Mary William EthelBert Appleton “Billieâ€; American performing artist (1884- 1970). Castiglione Giuseppe; Italian painter in the court of the Emperor of China (1688-1766). Driscoll Clara; American stained glass artist (1861-1944). Du Fu Tu Fu; Chinese poet (712-770). Heaney Seamus Justin; Irish poet and playwright (1939 - 2013). JoBim Antonio Carlos; Brazilian composer and musician (1927-1994). Kerouac Jack, American poet and author (1922-1969). Namatjira Albert; Australian Aboriginal artist, pioneer of contemporary Indigenous Australian art (1902-1959). Plath Sylvia; American poet (1932-1963). Sapkota Mahananda; Nepalese poet (1896-1977). Villa-LoBos Heitor; Brazilian composer (1887-1959). Vonnegut Kurt; American writer (1922-2007). Yamada Kosaku; Japanese composer and conductor (1886-1965). Planitiae (9) Apārangi Planitia Māori word for the planet Mercury. Lugus Planitia Gaulish equivalent of the Roman god Mercury. Mearcair Planitia Irish word for the planet Mercury. Otaared Planitia Arabic word for the planet Mercury. Papsukkal Planitia Akkadian messenger god. Sihtu Planitia Babylonian word for the planet Mercury. StilBon Planitia Ancient Greek word for the planet Mercury.