Venus": Venus Model with Feature Names

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"A TOUCH OF VENUS": VENUS MODEL WITH FEATURE NAMES by Amelia Ortiz-Gil (University oF Valencia Astronomical Observatory) “A Touch of Venus” is funded by the IAU OFFice oF Astronomy For Development (OAD). All materials have been produced under a Creative Commons Attribution- NonCommercial-ShareAlike 4.0 International License (CC BY-NC-SA 4.0) A Touch of the Universe - VENUS This is a tactile 3D model of the planet Venus made from topographical data obtained by NASA’s Magellan mission. The model was created using Jordi Burguet’s Mapelia software (https:// github.com/jordibc/mapelia). The North polar cap is smooth; the South Polar cap contains the logo of the University of Valencia Astronomical Observatory. The meridian corresponds to 0º longitude in the planet’s geographical coordinates. After tests, the best size for the globe has been found to be around 20 cm in diameter. Larger globes are cumbersome and smaller ones are confusing. The 3D model of Venus, the activity book and this document can be downloaded from the “A Touch of the Universe” website: https://astrokit.uv.es . A topographical interactive map of Venus can be found at https:// webgis2.wr.usgs.gov/Venus_Global_GIS/ The Venus model is part of “A Touch of the Universe”. It is licensed under the “A Touch Of the Universe” CC license: A Touch of the Universe by University of Valencia Astronomical Observatory is licensed under a Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International License. NORTH POLE Meridian 0 Maxwell Montes Sacajawea Patera FORTUNA TESSERA ISHTAR TERRA Fedorets Sigrun Fossae SEDNA PLANITIA Gula Mons Gautier Beyla Corona Mona Lisa Sif Mons Comnena TINATIN PLANITIA Sappho Patera Meridian 0 Mona Lisa Didilia Corona Pavlova Corona Sappho Patera TINATIN PLANITIA MANATUM TESSERA Vabuzana Corona TELLUS TESSERA Lemkechen Adivar Dorsa SOGOLON PLANITIA Joliot-Curie APHRODITE TERRA Bathsheba MANATUM TESSERA TAHMINA PLANITIA AINO PLANITIA Pioneer Venus Night Probe ANANKE TESSERA Maria Celeste TILLI-HANUM Greenaway PLANITIA VELLAMO PLANITIA SOGOLON PLANITIA RUSALKA CERES PLANITIA CORONA APHRODITE TERRA THETIS REGIO Quilla Chasma ATAHENSIK Diana Chasma CORONA ARTEMIS CORONA ZHIBEK PLANITIA Mahuea Tholus Ermolova ATALANTA PLANITIA GANIKI PLANITIA ATLA REGIO Sapas Mons Ozza Mons RUSALKA Dali Chasma PLANITIA Vega 1 Vega 2 Atahensik Corona Zemina Corona Mahuea Tholus ZHIBEK PLANITIA Boleyn Taranga Corona GANIKI PLANITIA Sapas Mons ULFRUN REGIO HINEMODA PLANITIA Atete Corona Maat Mons WAWALAG Ozza Mons PLANITIA Stanton Stowe Rhea Mons Theia Mons Sanger GUINEVERE PLANITIA Venera 9 Wheatley Taranga Corona BETA REGIO Rosa Bonheur UNDINE PLANITIA Tuulikki Mons Pioneer Venus HINEMOA Large Probe PLANITIA PHOEBE REGIO Dolya Tessera Venera 13 DZERASSA PLANITIA GUNDA PLANITIA Venera 14 Aurelia Seymour Atanua Mons Venera 8 VASILISA NAVKA PLANITIA REGIO Heng-o Corona Carson DIONE REGIO Aglaonice Saskia Pioneer Venus Day Probe Ushas Mons Morrigan Linea Meitner Carson Aglaonice ALPHA REGIO Danilova Stuart LADA TERRA Saskia Quetzalpetlatl Corona Freyja Montes Akna Montes Cleopatra LAKSHMI PLANUM Maxwell Montes SEDNA PLANITIA Sigrun Fossae.

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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
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Round 3 Michael Etzkorn • Brad Fischer • Clare Keenan • Mike Laudermith • Lauren Onel Noah Prince • Jacob Simmons • Kristin Strey • Tyler Vaughan
2017 SCOP MS 8 Round 3 Michael Etzkorn • Brad Fischer • Clare Keenan • Mike Laudermith • Lauren Onel Noah Prince • Jacob Simmons • Kristin Strey • Tyler Vaughan Tossups (1) This astronomical body, which was called Hesperus when it appeared as the Evening Star, has surface features called Maxwell Montes, Lakshmi Planum, and Ishtar Terra that are obscured by a permanent cover of (*) sulfuric acid clouds. A 96% carbon dioxide atmosphere led to a runaway greenhouse effect on, for ten points, what second planet in the Solar System? ANSWER: Venus (2) A holder of this title controversially pushed his people away from polytheism in favor of a solar god worshiped at Amarna. Lord Carnavon funded Howard Carter’s 1922 expedition to discover the burial grounds of one of these people at (*) Luxor, and found a sarcophagus containing a solid gold funerary mask and mummified remains. For ten points, name this title given to Akenhaten, King Tut, and other ancient Egyptian rulers. ANSWER: Egyptian pharaohs (3) A composer from this country wrote about the unlucky servant Ninetta in The Thieving Magpie, and included a “cavalry charge” galop in his (*) William Tell overture. For ten points, name this home country of Gioachino Rossini as well as Giacomo Puccini, who set his opera Tosca in Rome. ANSWER: Italy (accept Italia; accept Italian Republic or Repubblica italiana) (4) The Rydberg formula inspired one model of these objects, and the first sub-parts of these objects were detected by a deflection of cathode rays observed by JJ Thomson. A (*) gold foil experiment determined that these things possess a dense central mass, disproving their “plum pudding” model.
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Regional Geology of the Beta-Phoebe Region on Venus J. B. Garvin
REGIONAL GEOLOGY OF THE BETA-PHOEBE REGION ON VENUS. J. B. Garvin and J. W. Head, Oept. of Geological Sciences, Brown Univ. , Providence, RI 02912, and A, T. Basilevsky, Vernadsky Institute, USSR Academy of Sciences, Moscow, USSR.. The planet Venus is dominated by extensive rolling plains (6% of surface area) which serve to separate and isolate the highlands and lowlands. Of the three major highland regions on Venus, the Beta-Phoebe area is the most fully characterized, on the basis of the wealth and variety of data avai lable -- Earth-based radar images ( Areci bo , Goldstone). Venera lander panoramas (Veneras 8-14 landed east of these highlands), and corrplete Pioneer-Venus orbiter radar coverage. Neither Aphrodite nor Ishtar Terrae are covered as well as the Beta-Phoebe region; there has yet to be a lander mission to either of these highlands, though the Vega landers are targeted for an area near Aphrodite. The data available for Beta-Phoebe and the surrounding plains spans several or- ders of magnitude in resolution, from cm-scale in the Venera panoramas to several kin-scale in Earth-based radar backscatter images, to 30-100 km in Pioneer-Venus maps of radar roughness (a0), reflectivity (p), and altimetry (z). This affords us an opportunity to analyze the geology of the region from the surface (Venera panoramas) and from afar (radar), and allows us to assess how re- presentative the Venera lander sites are of the high plains and lower highlands for this part of Venus. In addition, the entire Beta-Phoebe area can be compared with planet-wide radar proper- ties.
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Stony Brook University
SSStttooonnnyyy BBBrrrooooookkk UUUnnniiivvveeerrrsssiiitttyyy The official electronic file of this thesis or dissertation is maintained by the University Libraries on behalf of The Graduate School at Stony Brook University. ©©© AAAllllll RRRiiiggghhhtttsss RRReeessseeerrrvvveeeddd bbbyyy AAAuuuttthhhooorrr... The Civic Virtue of Women in Quattrocento Florence A Dissertation Presented by Christine Contrada to The Graduate School in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in History Stony Brook University May 2010 Copyright by Christine Contrada 2010 Stony Brook University The Graduate School Christine Contrada We, the dissertation committee for the above candidate for the Doctor of Philosophy degree, hereby recommend acceptance of this dissertation. Dr. Alix Cooper – Dissertation Advisor Associate Professor, History Dr. Joel Rosenthal – Chairperson of Defense Distinguished Professor Emeritus, History Dr. Gary Marker Professor, History Dr. James Blakeley Assistant Professor, History St. Joseph’s College, New York This dissertation is accepted by the Graduate School. Lawrence Martin Dean of the Graduate School ii Abstract of the Dissertation The Civic Virtue of Women in Quattrocento Florence by Christine Contrada Doctor of Philosophy in History Stony Brook University 2010 Fifteenth century Florence has long been viewed as the epicenter of Renaissance civilization and a cradle of civic humanism. This dissertation seeks to challenge the argument that the cardinal virtues, as described by humanists like Leonardo Bruni and Matteo Palmieri, were models of behavior that only men adhered to. Elite men and women alike embraced the same civic ideals of prudence, justice, fortitude, and temperance. Although they were not feminists advocating for social changes, women like Alessandra Strozzi, Margherita Datini, and Lucrezia Tornabuoni had a great deal of opportunity to actively support their own interests and the interests of their kin within popular cultural models of civic virtue.
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N93"14373 : ,' Atmospheric Density, Collapse of Near-Rim Ejecta Into a Flow Crudely MAGELLAN PROJECT PROGRESS REPORT
106 lnternational Colloquium on Venus ment as observed on Venus [5,6]. Such a process accounts for the results in late-stage reworking, if not self-destruction, of ejecta long run-out flows consistently originating downrange in oblique faciescmplaced earlier.Surfaceexpressionshould includebedforrns impacts (i.e., oplmsite the missing ejecta sector) even if uphill from (e.g., meter-scale dunes and decicentlmeter-scale ripples) reflect- the crater rim. Atmospheric mflxflence and recovery winds deeoupled hag eddies created in the boundary layer at the surface. Because from the gradient-controlled basal run-out flow continues down- radar imaging indicates small-scale surface roughness (as well as range and produces wind streaks in the Ice of topographic highs. resolved surface features), regions affected by such long-lived low- Turbulence accompanying the basal density flows may also produce energy processes can extend to enormous distances. Such areas are wind streak patterns. Uprange the atmosphere is drawn in behind the not directly related to ejecta emplacement but reflect the almo- f'_reball(and enhancedby the impinging impactor wake), resulting spheric equivalent to distant seismic waves in the target. Late-stage in strong winds that will last at least as long as the time for crater atmospheric processes also include interactions with upper-level formation (i.e., minutes). Such winds can entrain and saltate surface winds. Deflection of the winds around the advancing/expanding materials as observed in laboratory experiments [2,3] and inferred fireball creates a parabolic-shaped interface aloft. This is preserved from large transverse dunes uprange on Venus [2]. in the fall-out of f'mer debris for impacts directed into the winds aloft Atmospheric Effects on Ballistic EJecta: Even on Venus, (from the west) but self-destructs if the impact is directed with the target debris will be ballistically ejected and form a conical ejecta wind.
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Winds in the Lower Cloud Level on the Nightside of Venus from VIRTIS-M (Venus Express) 1.74 Μm Images
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May 2, 2020 Live the Ucf Creed
UNIVERSITY OF CENTRAL FLORIDA COMMENCEMENT MAY 2, 2020 LIVE THE UCF CREED INTEGRITY I will practice and defend academic and personal honesty. SCHOLARSHIP I will cherish and honor learning as a fundamental purpose of my membership in the UCF community. COMMUNITY I will promote an open and supportive campus environment by respecting the rights and contributions of every individual. CREATIVITY I will use my talents to enrich the human experience. EXCELLENCE I will strive toward the highest standards of performance in any endeavor I undertake. UNIVERSITY OF CENTRAL FLORIDA | COMMENCEMENT | MAY 2, 2020 About the University of Central Florida The University of Central Florida is a bold, public research institution that is regularly ranked among the nation’s top 20 most innovative universities by U.S. News & World Report. With more than 69,500 students, UCF is one of the largest universities in the United States and is ranked as one of the best educational values in the nation by Forbes and Kiplinger. The university benefits from a diverse faculty and staff who create a welcoming environment and opportunities for all students to grow, learn, and succeed. A Foundation for Success UCF and its 13 colleges offer more than 220 degrees at UCF’s main campus, hospitality campus, health sciences campus, online and through multiple regional locations. The 1,415-acre main campus is 13 miles east of downtown Orlando and adjacent to one of the top research parks in the nation. Other campuses are located throughout Central Florida and include a fully accredited College of Medicine at Lake Nona.
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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.
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Cleopatra Crater on Venus: Happy Solution of the Volcanic Vs
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Styles of Deformation in Ishtar Terra and Their Implications
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User Guide to the Magellan Synthetic Aperture Radar Images
https://ntrs.nasa.gov/search.jsp?R=19950018567 2020-06-16T07:22:10+00:00Z User Guide to the Magellan Synthetic Aperture Radar Images Stephen D. Wall Shannon L. McConnell Craig E. Left Richard S. Austin Kathi K. Beratan Mark J. Rokey National Aeronautics and Jet Propulsion Laboratory Space Administration California Institute of Technology Scientific and Technical Pasadena, California Information Branch NASA Reference Publication 1356 March 1995 This publication was prepared at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Contents Iri Introduction .................................................................................................................................................................... 1 I_1 The Spacecraft ................................................................................................................................................................ 2 IB Mission Design ................................................................................................................................................................ 4 D Experiment Description ................................................................................................................................................ 15 B Mission Operations ....................................................................................................................................................... 17 [] Notable Events and Problems .....................................................................................................................................
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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.
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