Presentazione Di Powerpoint
Total Page：16
File Type：pdf, Size：1020Kb
Load more
Recommended publications
-
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 -
GEOLOGY of OVDA REGIO, APHRODITE TERRA, VENUS: Prelih4inar-Y RESULTS from MAGELLAN DATA, RS
LPSC SSII 1169 GEOLOGY OF OVDA REGIO, APHRODITE TERRA, VENUS: PRELIh4INAR-Y RESULTS FROM MAGELLAN DATA, RS. Saundersl, J.W. Head m2,RJ. Phillips3, S.C. Solomon4, R. Herricl?, R. Grimm3, and E.R. Stofan1 Jet Propulsion Laboratory, Calif. Institute of Technology, Pasadena, CA 91109;%epartment of Geological Sciences, Brown University, Providence, RI 02912; 3Southern Methodist University, Dallas, TX 75275;'Massachusetts Institute of Technology, Cambridge, MA, 02139 Ovda Regio is located in Aphrodite Terra, a major highland region on Venus which straddles the equator between 75 and 100 degrees east longitude. Ovda is located in western Aphrodite Terra, and has now been mapped by the Magellan spacecraft. The morphology of highland regions on Venus varies from a high plateau surrounded by mountain belts in Ishtar Terra [1,2], highly deformed tessera terrain in Tellus and Alpha Regiones [3, 41 to volcanism and rifting in Beta Regio [S-71. Aphrodite Terra, previously imaged only by low resolution Pioneer Venus radar, has been the subject of much speculation, and is expected to reveal important information on the formation and evolution of highland terrains on Venus. Pioneer Venus topography indicates that Ovda is a 2000 x 3500 km highland region rising over 4 km above the surroundink plains. Its interior is relatively plateau-like, with steep outer margins. Pioneer Venus roughness and reflectivity data indicated that the surface may be composed of tessera-like terrain [8], while PVO gravity data gave a relatively shallow depth of compensation at Ovda [9]. Several theories have been proposed for Ovda Regio based on Pioneer Venus data. -
Investigating Mineral Stability Under Venus Conditions: a Focus on the Venus Radar Anomalies Erika Kohler University of Arkansas, Fayetteville
University of Arkansas, Fayetteville ScholarWorks@UARK Theses and Dissertations 5-2016 Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies Erika Kohler University of Arkansas, Fayetteville Follow this and additional works at: http://scholarworks.uark.edu/etd Part of the Geochemistry Commons, Mineral Physics Commons, and the The unS and the Solar System Commons Recommended Citation Kohler, Erika, "Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies" (2016). Theses and Dissertations. 1473. http://scholarworks.uark.edu/etd/1473 This Dissertation is brought to you for free and open access by ScholarWorks@UARK. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of ScholarWorks@UARK. For more information, please contact [email protected], [email protected]. Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Space and Planetary Sciences by Erika Kohler University of Oklahoma Bachelors of Science in Meteorology, 2010 May 2016 University of Arkansas This dissertation is approved for recommendation to the Graduate Council. ____________________________ Dr. Claud H. Sandberg Lacy Dissertation Director Committee Co-Chair ____________________________ ___________________________ Dr. Vincent Chevrier Dr. Larry Roe Committee Co-chair Committee Member ____________________________ ___________________________ Dr. John Dixon Dr. Richard Ulrich Committee Member Committee Member Abstract Radar studies of the surface of Venus have identified regions with high radar reflectivity concentrated in the Venusian highlands: between 2.5 and 4.75 km above a planetary radius of 6051 km, though it varies with latitude. -
Geologic Investigations Series I-2808
Prepared for the National Aeronautics and Space Administration Geologic Map of the Ovda Regio Quadrangle (V–35), Venus By Leslie F. Bleamaster, III, and Vicki L. Hansen Pamphlet to accompany Geologic Investigations Series I–2808 75° 75° V–1 V–2 V–4 50° 50° V–3 V–8 V–13 V–9 V–12 V–10 V–11 25° 25° V–20 V–25 V–21 V–24 V–22 V–23 0° 30° 60° 90° 120° 150° 180° 0° 0° V–34 V–35 V–33 V–36 V–32 V–37 –25° –25° V–46 V–47 V–45 V–48 V–44 V–49 V–57 –50° V–56 V–58 –50° V–62 2005 –75° –75° U.S. Department of the Interior U.S. Geological Survey 0 THE MAGELLAN MISSION comparable to the radar wavelength are responsible for variations in the SAR return. In either case, the echo The Magellan spacecraft orbited Venus from August strength is also modulated by the reflectivity of the sur- 10, 1990, until it plunged into the Venusian atmosphere face material. The density of the upper few wavelengths on October 12, 1994. Magellan had the objectives of (1) of the surface can have a significant effect. Low-density improving knowledge of the geologic processes, surface layers, such as crater ejecta or volcanic ash, can absorb properties, and geologic history of Venus by analysis of the incident energy and produce a lower observed echo. surface radar characteristics, topography, and morphol- On Venus, a rapid increase in reflectivity exists at a cer- ogy and (2) improving knowledge of the geophysics of tain critical elevation, above which high-dielectric miner- Venus by analysis of Venusian gravity. -
The Magellan Spacecraft at Venus by Andrew Fraknoi, Astronomical Society of the Pacific
www.astrosociety.org/uitc No. 18 - Fall 1991 © 1991, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112. The Magellan Spacecraft at Venus by Andrew Fraknoi, Astronomical Society of the Pacific "Having finally penetrated below the clouds of Venus, we find its surface to be naked [not hidden], revealing the history of hundreds of millions of years of geological activity. Venus is a geologist's dream planet.'' —Astronomer David Morrison This fall, the brightest star-like object you can see in the eastern skies before dawn isn't a star at all — it's Venus, the second closest planet to the Sun. Because Venus is so similar in diameter and mass to our world, and also has a gaseous atmosphere, it has been called the Earth's "sister planet''. Many years ago, scientists expected its surface, which is perpetually hidden beneath a thick cloud layer, to look like Earth's as well. Earlier this century, some people even imagined that Venus was a hot, humid, swampy world populated by prehistoric creatures! But we now know Venus is very, very different. New radar images of Venus, just returned from NASA's Magellan spacecraft orbiting the planet, have provided astronomers the clearest view ever of its surface, revealing unique geological features, meteor impact craters, and evidence of volcanic eruptions different from any others found in the solar system. This issue of The Universe in the Classroom is devoted to what Magellan is teaching us today about our nearest neighbor, Venus. Where is Venus, and what is it like? Spacecraft exploration of Venus's surface Magellan — a "recycled'' spacecraft How does Magellan take pictures through the clouds? What has Magellan revealed about Venus? How does Venus' surface compare with Earth's? What is the next step in Magellan's mission? If Venus is such an uninviting place, why are we interested in it? Reading List Why is it so hot on Venus? Where is Venus, and what is it like? Venus orbits the Sun in a nearly circular path between Mercury and the Earth, about 3/4 as far from our star as the Earth is. -
The Earth-Based Radar Search for Volcanic Activity on Venus
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 2339.pdf THE EARTH-BASED RADAR SEARCH FOR VOLCANIC ACTIVITY ON VENUS. B. A. Campbell1 and D. B. Campbell2, 1Smithsonian Institution Center for Earth and Planetary Studies, MRC 315, PO Box 37012, Washington, DC 20013-7012, [email protected]; 2Cornell University, Ithaca, NY 14853. Introduction: Venus is widely expected to have geometry comes from shifts in the latitude of the sub- ongoing volcanic activity based on its similar size to radar point, which spans the range from about 8o S Earth and likely heat budget. How lithospheric (2017) to 8o N (2015). Observations in 1988, 2012, and thickness and volcanic activity have varied over the 2020 share a similar sub-radar point latitude of ~3o S. history of the planet remains uncertain. While tessera Coverage of higher northern and southern latitudes may highlands locally represent a period of thinner be obtained during favorable conjunctions (Fig. 1), but lithosphere and strong deformation, there is no current the shift in incidence angle must be recognized in means to determine whether they formed synchronously analysis of surface features over time. The 2012 data on hemispheric scales. Understanding the degree to were collected in an Arecibo-GBT bistatic geometry which mantle plumes currently thin and uplift the crust that led to poorer isolation between the hemispheres. to create deformation and effusive eruptions will better inform our understanding of the “global” versus Searching for Change. Ideally, surface change “localized” timing of heat transport. Ground-based detection could be achieved by co-registering and radar mapping of one hemisphere of Venus over the past differencing any pair of radar maps. -
Westfield Council Approves Budget (Continued from Page A-L) Sullivan Also Thanked State Two More Years," Said Echausse
Cook's walk-off homer lifts WHS past Union. Please see Sports, Page C-1. WESTFIELD SCOTCH PLAINS FANWOOD Vol. 16, No.' Friday, April 27, 2001 50 cents Aro Small businesses have a friend in county corporation By GREG MARX For loans or training, the UCEDC is there for the little guys Trustees with members from "all Tow THE RECORD-PRESS walks of life," Brown said. The Bonn! of Trustees offers guidance Westfield wel< UNION COUNTY — In mod- an important ally in the Union "our key goal is to assist smiill- under-served groups, such as on how the UCEDC can best dis- ern suburban communities, small County Economic Development and medium-size businesses in women and minority entrepre- tribute the funds it collects from TV-36broadc downtown businesses often Corporation. low- to moderate-income areas." neurs. fund-raising activities and WESTHEtti struggle to compete with huge According to Susan Brown, In more affluent areas, Brown To undertake that task, the grunts from county and federal access televisi' chain stores on regional high- director of Business said, the UCEDC seeks to help UCEDC lias a paid staff of 12 agencies. launched a new ways. But local businesses have Development for the UCEDC, individuals from historically and a volunteer Board of (Continued on page A-8) night with a ril thenewTV-36br The center is second floor of the Westfield Westfield council Municipal Building and will replace space previously occu- pied at Westfield High School. Phil Falcone, chairman of the TV- 36 Advisory Committee, said offi- approves budget cials hope the new center will enhance broadcasts over the a whole cent, according to town cable-access channel. -
Final Report Venus Exploration Targets Workshop May 19–21
Final Report Venus Exploration Targets Workshop May 19–21, 2014, Lunar and Planetary Institute, Houston, TX Conveners: Virgil (Buck) Sharpton, Larry Esposito, Christophe Sotin Breakout Group Leads Science from the Surface Larry Esposito, Univ. Colorado Science from the Atmosphere Kevin McGouldrick, Univ. Colorado Science from Orbit Lori Glaze, GSFC Science Organizing Committee: Ben Bussey, Martha Gilmore, Lori Glaze, Robert Herrick, Stephanie Johnston, Christopher Lee, Kevin McGouldrick Vision: The intent of this “living” document is to identify scientifically important Venus targets, as the knowledge base for this planet progresses, and to develop a target database (i.e., scientific significance, priority, description, coordinates, etc.) that could serve as reference for future missions to Venus. This document will be posted in the VEXAG website (http://www.lpi.usra.edu/vexag/), and it will be revised after the completion of each Venus Exploration Targets Workshop. The point of contact for this document is the current VEXAG Chair listed at ABOUT US on the VEXAG website. Venus Exploration Targets Workshop Report 1 Contents Overview ....................................................................................................................................................... 2 1. Science on the Surface .............................................................................................................................. 3 2. Science within the Atmosphere ............................................................................................................... -
Ooooooooo ° °
LPI Contribution No. 789 57 highest basal elevation, Maat Mons, should have a well-developed, large, and relatively deeper NBZ and that the volcano at the lowest 6055 .It .... _ .... _ .... t .... t .... I .... altitude, an unnamed volcano located southwest of Beta Regio at 10 °, 273 °, should have either a poorly developed magma chamber 6054 _ o _ o or none at all [2]. Preliminary mapping of Mast Mons [3] identified o at least six flow units that exhibit greater variations in morphology ._ o o o and radar properties than the flow• of Saps• Mons. These units are 6053 o 8 o also spatially and temporally distinct and suggest the eruption of a continuously evolving magma. Although smaller in diameter, the o oo o summit c.alders is much bener defined than the depression at Saps•. The inferred young age of Mast (lOose et at. [4] suggest that it may ooooooooo° ° ° I even be "active") may mean that the chamber has not yet grown to 605tj#o_o o 6050_ .... t", ', _ .... _ ", • i • i ' "full size." explaining the relatively smaller caldera. There is no 0 1 2 3 4 5 6 evidence of radial fractures at Maat Mons, suggesting that if lateral Height (kin) dike propagation occurxed, it was sufficiently deep that there was no surface expression. In contrast, the unnamed volcano has no summit features, no radial dikes, and only three flow units that exhibit Fig. 3. Graph showing the heights of ! l0 large volcanos as • function of considerable morphologic variations within units [3]. These obser- basal altitude. -
Geological Evolution of Lada Terra, Venus
42nd Lunar and Planetary Science Conference (2011) 1090.pdf GEOLOGICAL EVOLUTION OF LADA TERRA, VENUS. P. Senthil Kumar 1,2 and James W. Head 2, National Geophysical Research Institute, CSIR, Hyderabad 500606, India ([email protected]); 2Department of Geological Sciences, Brown University, Providence, RI02912, USA ([email protected]) Introduction: In this study, we present the history depict outflow features inundating the ejecta deposits. of geologic processes at Lada Terra (V-56 Quadrangle) Lineaments are abundant in V-56. These are in the southern hemisphere of Venus, through geologic principally secondary deformation features such as mapping at 1:5,000,000 scale, using 250-m-per-pixel fractures, faults, grabens, linear ridges, and wrinkle Magellan SAR image and ArcGIS 9.3 software, ridges. In V-56, there are three concentric coronae following the methods of geologic unit definition and (e.g., Quetzalpetlatl, Eithinaho, and Serpantium), one characterization of planetary surfaces [1-3]. Geological double ringed corona (Otygen), seven asymmetric units in the V-56 were products of tectonics, coronae (e.g., Derceto, Demvamvit, Toyo-uke, volcanism, and impact cratering with characteristic Dyamenyuo and Ekhe-Burkhan) and one astra-like geomorphic expressions (Figure 1). Basically, this structure (Loo-Wit Mons). Radial and concentric quadrangle addresses how coronae evolved in fractures and grabens define the coronae structures. association with regional extensional belts, in addition The large extensional belts are composed of fractures, to evolution of tessera, regional plains and impact grabens and strike-slip zones. The most prominent craters, which are also significant geological units of tectonic features are the traverses of four large-scale Lada Terra. -
Observational Constraints on Venus Surface Composition and Geologic History
Comparative Tectonics and Geodynamics (2015) 5025.pdf OBSERVATIONAL CONSTRAINTS ON VENUS SURFACE COMPOSITION AND GEOLOGIC HISTORY. M. S. Gilmore, Dept. Earth & Environmental Sciences, Wesleyan University, 265 Church St., Mid- dletown CT 06457 [email protected], www.wesleyan.edu/planetary. Introduction: The Venus atmosphere precludes hematite, the high emissivity anomalies correspond to the visible-near-infrared hyperspectral observations more mafic (less weathered) compositions [10] and the that have revolutionized the study of the surface com- low emissivity anomalies correspond to more felsic position of mars, Mercury and the Moon. Our under- compositions [7, 9, 11]. If the weathering rate of bas- standing of the surface composition the Earth-sized alt to hematite is fast, this suggests the volcanoes are planet Venus is derived wholly from 1) geochemical geologically young [10]. analyses of rocks from 7 landing sites, 2) observations Tesserae – How felsic? The radiance flux corre- of the surface at 1µm through a spectral window in the sponds to low emissivity values for tessera terrain atmosphere. These data are supported by theoretical leading to the following radical conclusions about Ve- and laboratory studies of the weathering, rheology and nus: 1) tesserae have a different (more felsic, less fer- spectra of candidate rocks at Venus temperatures and rous) primary composition. This can include Archean atmospheric composition. – type (TTG) granites formed by dehydration of under- Bulk Composition: The Venera and Vega landers thrust slabs or the lower crust, or true granites which acquired drilled samples (rock + soil) at 7 locations on may require a mature global recycling mechanism in- Venus. Major elements were measured by XRF at 3 troducing water-rich rocks. -
VENUS Corona M N R S a Ak O Ons D M L YN a G Okosha IB E .RITA N Axw E a I O
N N 80° 80° 80° 80° L Dennitsa D. S Yu O Bachue N Szé K my U Corona EG V-1 lan L n- H V-1 Anahit UR IA ya D E U I OCHK LANIT o N dy ME Corona A P rsa O r TI Pomona VA D S R T or EG Corona E s enpet IO Feronia TH L a R s A u DE on U .TÜN M Corona .IV Fr S Earhart k L allo K e R a s 60° V-6 M A y R 60° 60° E e Th 60° N es ja V G Corona u Mon O E Otau nt R Allat -3 IO l m k i p .MARGIT M o E Dors -3 Vacuna Melia o e t a M .WANDA M T a V a D o V-6 OS Corona na I S H TA R VENUS Corona M n r s a Ak o ons D M L YN A g okosha IB E .RITA n axw e A I o U RE t M l RA R T Fakahotu r Mons e l D GI SSE I s V S L D a O s E A M T E K A N Corona o SHM CLEOPATRA TUN U WENUS N I V R P o i N L I FO A A ght r P n A MOIRA e LA L in s C g M N N t K a a TESSERA s U . P or le P Hemera Dorsa IT t M 11 km e am A VÉNUSZ w VENERA w VENUE on Iris DorsaBARSOVA E I a E a A s RM A a a OLO A R KOIDULA n V-7 s ri V VA SSE e -4 d E t V-2 Hiei Chu R Demeter Beiwe n Skadi Mons e D V-5 S T R o a o r LI s I o R M r Patera A I u u s s V Corona p Dan o a s Corona F e A o A s e N A i P T s t G yr A A i U alk 1 : 45 000 000 K L r V E A L D DEKEN t Baba-Jaga D T N T A a PIONEER or E Aspasia A o M e s S a (1 MM= 45 KM) S r U R a ER s o CLOTHO a A N u s Corona a n 40° p Neago VENUS s s 40° s 40° o TESSERA r 40° e I F et s o COCHRAN ZVEREVA Fluctus NORTH 0 500 1000 1500 2000 2500 KM A Izumi T Sekhm n I D .