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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. -
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. -
Cleopatra Crater on Venus: Happy Solution of the Volcanic Vs
CLEOPATRA CRATER ON VENUS: HAPPY SOLUTION OF THE VOLCANIC VS. IMPACT CRATER CONTROVERSY; A.T. Basilevsky, A.T. Vernadsky Institute of Geochemistry and Analytical chemistry, Moscow, USSR, and G.G. Schaber, U.S. Geological Survey, Flagstaff AZ 86001 ~ntroduction. Cleopatra is a 100-km-diameter crater on the eastern slope of Maxwell Montes in western Ishtar Terra. For over 12 years, Cleopatra has been the subject of scientific controversy. Discovered during the Pioneer Venus altimetric survey, this feature was initially interpreted as a caldera near the top of a giant volcanic construct, Maxwell Montes [I]. Venera 15/16 data and recent Arecibo radar images show, however, that the Maxwell Montes appear to be more of a tectonic construct, with little or no resemblance to other giant shields known in the Solar System; thus, a nonvolcanic origin of Cleopatra was proposed [2-61. The similarity of the double-ring structure of Cleopatra to those of other multi-ring impact craters of similar size on Venus and the Moon, Mercury, and Mars was more recently given by Basilevsky and Ivanov [7] as the primarily reason to consider this feature an impact crater. At the same time, some characteristics of Cleopatra seemed to contradict an impact origin. For example, Schaber et al. [8], suggestingthat a definitive verification of a volcanic or impact origin would probably require Magellan data, proposed that the evidence from Venera 15/16 and earlier data for a probable volcanic origin for Cleopatra is substantial. They cited, among other points: (1) the absence of a raised rim and highly backscattering ejecta deposits; (2) the crater's association with plains-forming deposits immediately downslope to the east, interpreted as probable lava flows emanating from a distinct breach in the crater's rim; (3) the excessive depth (2.5 km) and depth-to-diameter ratio (0.028) of the crater, (4) the offset of the inner and outer craters; and (5) the crater's position in what was interpreted as a regional tectonic framework. -
Styles of Deformation in Ishtar Terra and Their Implications
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 97, NO. El0, PAGES 16,085-16,120, OCTOBER 25, 1992 Stylesof Deformationin IshtarTerra and Their Implications Wn.T.TAMM. KAU•A,• DOAN•L. BINDSCHAD•-R,l ROBERT E. GPaM•,2'3 VICKIL. HANSEN,2KARl M. ROBERTS,4AND SUZANNE E. SMREr,AR s IshtarTerra, the highest region on Venus, appears to havecharacteristics of both plume uplifts and convergent belts.Magellan imagery over longitudes 330ø-30øE indicates a great variety of tectonicand volcanic activity, with largevariations within distances of onlya few 100km. Themost prominent terrain types are the volcanic plains of Lakshmiand the mountain belts of Maxwell,Freyja, and Danu. Thebelts appear to havemarked variations in age. Thereare also extensive regions of tesserain boththe upland and outboard plateaus, some rather featureless smoothscarps, flanking basins of complexextensional tectonics, and regions of gravitationalor impactmodifica- tion.Parts of Ishtarare the locations of contemporaryvigorous tectonics and past extensive volcanism. Ishtar appearsto be the consequence of a history of several100 m.y., in whichthere have been marked changes in kinematic patternsand in whichactivity at any stage has been strongly influenced by the past. Ishtar demonstrates three general propertiesof Venus:(1) erosionaldegradation is absent,leading to preservationof patternsresulting from past activity;(2) manysurface features are the responses ofa competentlayer less than 10 km thick to flowsof 100km orbroaderscale; and (3) thesebroader scale flows are controlled mainly by heterogeneities inthe mantle. Ishtar Terra doesnot appear to bethe result of a compressionconveyed by anEarthlike lithosphere. But there is stilldoubt as to whetherIshtar is predominantlythe consequence of a mantleupflow or downflow.Upflow is favoredby the extensivevolcanic plain of Lakshmiand the high geoid: topography ratio; downflow is favoredby the intense deformationof themountain belts and the absence of majorrifts. -
Venus' Ishtar Terra: Topographic Analysis of Maxwell, Freyja, Akna
16th VEXAG Meeting 2018 (LPI Contrib. No. 2137) 8046.pdf Venus’ Ishtar Terra: Topographic Analysis of Maxwell, Freyja, Akna and Danu Montes. Sara Rastegar1 and 2 1 Donna M. Jurdy , C ity Colleges of Chicago, Harold Washington College, 30 E. Lake Street, Chicago, IL 60601, 2 [email protected], D epartment of Earth and Planetary Sciences, Northwestern University, 2145 Sheridan Rd, Evanston, IL 60208, [email protected] Introduction: Venus’ mountain chains (Figure 1) Analysis: We attempt to address these questions surround Lakshmi Planum, a 3-4 km highland, making with analysis of Magellan topographic data for up Ishtar Terra. No other mountain belts exist on quantitative comparison of Venus' four mountain Venus. Circling Ishtar Terra, Maxwell Montes, ascends chains: Maxwell, Freyja, Akna and Danu. Patterns in to over 11 km, ranking as the location of highest topography may provide clues to the dynamics forming elevation on the planet. Freyja Montes rises to over 7 these Venusian orogenic belts. From topographic km, higher than Akna Montes at about an elevation of profiles across the ec mountain chain, we then 6 km. Danu Montes, ~1.5 km over Lakshmi Planum, determine an average profile for each mountain belt. alone displays a distinctly arcuate form. Next, we correlate these averages to establish a measure of similarity between the chains and terrestrial Tectonic Enigma: The existence of the four analogs. These correlations allow construction of a venusian mountain chains has been attributed to covariance matrix, which can be diagonalized for localized downwelling - analogous to terrestrial eigenvalues, for Principal Component Analysis (PCA) subduction - in response to the proposed upwelling [4]. -
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. -
Testing Evolutionary Models for Venus with the DAVINCI+ Mission
EPSC Abstracts Vol. 14, EPSC2020-534, 2020 https://doi.org/10.5194/epsc2020-534 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Venus, Earth's divergent twin?: Testing evolutionary models for Venus with the DAVINCI+ mission Walter S. Kiefer1, James Garvin2, Giada Arney2, Sushil Atreya3, Bruce Campbell4, Valeria Cottini2, Justin Filiberto1, Stephanie Getty2, Martha Gilmore5, David Grinspoon6, Noam Izenberg7, Natasha Johnson2, Ralph Lorenz7, Charles Malespin2, Michael Ravine8, Christopher Webster9, and Kevin Zahnle10 1Lunar and Planetary Institute/USRA, Houston, Texas, United States of America ([email protected]) 2NASA Goddard Space Flight Center, Greenbelt MD USA 3Planetary Science Laboratory, University of Michigan, Ann Arbor MI USA 4Center for Earth and Planetary Studies, Smithsonian Institution, Washington DC USA 5Dept. of Earth and Environmental Science, Wesleyan University, Middletown CT USA 6Planetary Science Institute, Tucson AZ USA 7Applied Physics Lab, Johns Hopkins University, Laurel MD USA 8Malin Space Science Systems, San Diego CA USA 9Jet Propulsion Laboratory, California Insitute of Technology, Pasadena CA USA 10NASA Ames Research Center, Moffet Field CA USA Understanding the divergent evolution of Venus and Earth is a fundamental problem in planetary science. Although Venus today has a hot, dry atmosphere, recent modeling suggests that Venus may have had a clement surface with liquid water until less than 1 billion years ago [1]. Venus today has a nearly stagnant lithosphere. However, Ishtar Terra’s folded mountain belts, 8-11 km high, morphologically resemble Tibet and the Himalaya mountains on Earth and apparently require several thousand kilometers of surface motion at some time in Venus’s past. -
Treatise on the Decorative Part Civil Architecture
TREATISE O N TH E D EC O R ATI V E P A RT CIV IL ARCH ITECTURE , S IR W I IA HA E S LL M C M B R , K.P.S. F.R.S. P.S.A. WITH I LLUSTRA TI N S N O , OTES , A N D AN EX AMI N ATI ON G C N CH C U RE I A AR I T E T RE , EPH WILT ARCHITECT F.S.A. JOS G , , LON D ON PRIESTLEY AN D WEALE. MDCCCX X V . CON TEN TS . DEDICATI ON Listof Subscribers Prefac e to thi s Edi tion Life of Sir Willi am Chambers Of the Elements of Beauty i n Archi te cture Of the Origin of Grecian Archi te cture Of the Progress an d Perfection of Gre cian Archi tecture D edi ca tion to the Thi rd Edition Preface to the Third Edi tion Introduction Of the Origin an d Progress of Buildi ng Of the Parts whi h om ose th e Orders of Ar hi te t re an d of c c p c c u , their Pro erties A li ation an d Enri hments p , pp c , c Of the Orders of Archi te cture in gen eral Of the Tus can Order Of the Doric Order Of the Ioni c Order Of the Composite Order Of the Corinthi an Order Of Pilasters Of P ersian s an d Caryatides Of Pede stals Of the Appli ca tion of the Orders of Architecture Of In tercolum ni ation s Of Arca des an d Arches Of Orders above Orders Of Basements an d Attics Of Pedi m en ts Of Balustra des Of ates Doors an d iers G , , P Of Win dows Of N iches an d Statues. -
The Science Return from Venus Express the Science Return From
The Science Return from Venus Express Venus Express Science Håkan Svedhem & Olivier Witasse Research and Scientific Support Department, ESA Directorate of Scientific Programmes, ESTEC, Noordwijk, The Netherlands Dmitri V. Titov Max Planck Institute for Solar System Studies, Katlenburg-Lindau, Germany (on leave from IKI, Moscow) ince the beginning of the space era, Venus has been an attractive target for Splanetary scientists. Our nearest planetary neighbour and, in size at least, the Earth’s twin sister, Venus was expected to be very similar to our planet. However, the first phase of Venus spacecraft exploration (1962-1985) discovered an entirely different, exotic world hidden behind a curtain of dense cloud. The earlier exploration of Venus included a set of Soviet orbiters and descent probes, the Veneras 4 to14, the US Pioneer Venus mission, the Soviet Vega balloons and the Venera 15, 16 and Magellan radar-mapping orbiters, the Galileo and Cassini flybys, and a variety of ground-based observations. But despite all of this exploration by more than 20 spacecraft, the so-called ‘morning star’ remains a mysterious world! Introduction All of these earlier studies of Venus have given us a basic knowledge of the conditions prevailing on the planet, but have generated many more questions than they have answered concerning its atmospheric composition, chemistry, structure, dynamics, surface-atmosphere interactions, atmospheric and geological evolution, and plasma environment. It is now high time that we proceed from the discovery phase to a thorough -
The Geologic Evolution of Venus: Insights Into Earth History
The geologic evolution of Venus: Insights into Earth history James W. Head Department of Geological Sciences, Brown University, Providence, Rhode Island 02912, USA Through the clever use of stereo radargrammetric techniques on im- Higher-resolution radar imaging and more coverage were needed to fi nd ages from the Magellan mission to Venus in the 1990s, combined with out whether Venus was Earth-like. recent quantitative analyses of magma reservoirs on Earth, McGovern et In 1983, Soviet Union orbiters Venera 15 and 16 surveyed the north- al. (2014, p. 59 in this issue of Geology) resolve an important outstanding ern hemisphere (~30% of Venus), with radar imaging resolution of 1–2 km question dating from that era: What forces are responsible for the graben (Barsukov et al., 1992), showing that many highlands consist of very high- extending radially from large shield volcanoes? They show that, in addi- ly deformed terrain (tesserae), and that organized linear folded mountain tion to radial dike emplacement, the larger graben are readily accounted belts surround highland plateaus. Large volcanoes exist in abundance, but for by magma reservoir infl ation, providing new insight into processes of show little evidence for hot spot traces or convergent plate boundaries. magma ascent and eruption on Venus, and their relation to globally inter- Coronae looked like the fi ngerprints of mantle processes. Most remark- connected rift systems on Earth’s sibling planet. This new contribution ably, there were few impact craters, indicating an age on the order of only serves as a reminder of the importance of Venus to our understanding of hundreds of millions of years. -
Nightwatch PVAA Gen Meeting 02/26/16 PVAA Officers and Board
Carl Sagan If you wish to make an apple pie from scratch, scratch, from pie an apple make to wish If you universe. the invent first must you Volume 36 Number 3 nightwatch March 2016 PVAA Gen Meeting 02/26/16 The Claremont Library is adding a third telescope to its was 12 separate areas of the galaxy seamlessly stitched together collection. You can check out the telescope for a week at a time. for a 5800 x 7700 pixel masterpiece. The photographer used the This telescope is a duplicate of the other two currently available. Slooh 17 inch reflector with a 2939mm focal length (f/6.8). 623 “Available” means you can check them out of the library, just exposures were stitched together to create the final image. like a book, but there is a waiting list that you would be put on. Eldred Tubbs brought in a graph showing gravity waves, and As the list is several (almost 6) months long, the 3rd telescope had a small presentation of what they had to go through to detect will, hopefully, reduce the wait. Many library patrons, after these waves. returning the telescope back to the library, immediately put their On a separate note, the April issue of Sky & Telescope has names back on the waiting list. Without a doubt, the Library an article entitled “Big Fish, Small Tackle” (Grab your Telescopes are a big hit. The PVAA maintains the telescopes, binoculars and drop a line in the deep pool of the Virgo Galaxy making sure they are kept in working order. -
Printed Books, Maps and Photographs , Oxford, Tuesday 25 and Wednesday 26 March 2014
Printed Books, Maps and Photographs , Maps and Photographs , Books, Printed Bonhams Banbury Road Shipton on Cherwell Kidlington Oxford OX5 1JH +44 (0) 1865 853 640 +44 (0) 1865 372 722 fax Oxford, Tuesday 25 and Wednesday 26 March 2014 Printed Books, Maps and Photographs Tuesday 25 March and Wednesday 26 March 2014 Oxford 21737 International Auctioneers and Valuers - bonhams.com Printed Books, Maps and Photographs Tuesday 25 March and Wednesday 26 March at 11am Oxford Bonhams Enquiries Shipping and Collections Banbury Road Shipton on Cherwell Oxford Oxford Kidlington John Walwyn-Jones Georgina Roberts Oxford OX5 1JH Georgina Roberts +44 (0) 1865 853 647 bonhams.com Sian Wainwright +44 (0) 1865 853 646 London Viewing +44 (0) 1865 853 647 Lydia Wilkinson Saturday 22 March 9am to 12pm +44 (0) 1865 853 648 +44 (0) 20 7393 3841 Monday 24 March 9am to 4.30pm Limited viewing on day of sale London Please see back of catalogue Matthew Haley for important notices to bidders Bids Luke Batterham +44(0) 20 7447 7448 Simon Roberts Illustrations +44(0) 20 7447 7401 fax Claire Wilkins Front cover: Lot 766 To bid via the internet Back cover: Lot 475 please visit www.bonhams.com +44 (0) 20 7393 3828 Contents: Lot 440 +44 (0) 20 7393 3879 fax Please note that bids should be [email protected] Sale number: 21737 submitted no later than 24 hours prior to the sale. Carole Park Catalogue: £18 +44 (0) 20 7393 3810 New bidders must also provide proof of identity when submitting Customer Services bids. Failure to do this may result in Monday to Friday 8.30am to 6pm your bids not being processed.