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Cumulated Bibliography of Biographies of Ocean Scientists Deborah Day, Scripps Institution of Oceanography Archives Revised December 3, 2001
Cumulated Bibliography of Biographies of Ocean Scientists Deborah Day, Scripps Institution of Oceanography Archives Revised December 3, 2001. Preface This bibliography attempts to list all substantial autobiographies, biographies, festschrifts and obituaries of prominent oceanographers, marine biologists, fisheries scientists, and other scientists who worked in the marine environment published in journals and books after 1922, the publication date of Herdman’s Founders of Oceanography. The bibliography does not include newspaper obituaries, government documents, or citations to brief entries in general biographical sources. Items are listed alphabetically by author, and then chronologically by date of publication under a legend that includes the full name of the individual, his/her date of birth in European style(day, month in roman numeral, year), followed by his/her place of birth, then his date of death and place of death. Entries are in author-editor style following the Chicago Manual of Style (Chicago and London: University of Chicago Press, 14th ed., 1993). Citations are annotated to list the language if it is not obvious from the text. Annotations will also indicate if the citation includes a list of the scientist’s papers, if there is a relationship between the author of the citation and the scientist, or if the citation is written for a particular audience. This bibliography of biographies of scientists of the sea is based on Jacqueline Carpine-Lancre’s bibliography of biographies first published annually beginning with issue 4 of the History of Oceanography Newsletter (September 1992). It was supplemented by a bibliography maintained by Eric L. Mills and citations in the biographical files of the Archives of the Scripps Institution of Oceanography, UCSD. -
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. -
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. -
The Official Journal of the Institute of Science & Technology – The
The Institute of Science & Technology The Institute of Science & Technology The Journal The Journal Winter 2011 Winter 2011 Kingfisher House 90 Rockingham Street Sheffield S1 4EB Tel: 0114 276 3197 [email protected] www.istonline.org.uk The Official Journal of The Institute of Science & Technology – The Professional Body for Specialist, Technical and Managerial Staff ISSN 2040-1868 The Journal The Official Publication of the Institute of Science & Technology ISSN 2040-1868 CONTENTS – Winter 2011 Editorial Ian Moulson Acting Chairman’s Report Terry Croft Letters to the Editor Rosina K Nyarko Astrobiology Colin Neve An inside view of a Venezuelan shrimp farm Carlos Conroy Origins, part 2: the general theory of relativity Estelle Asmodelle “My Lunar Estate”: the life of Hannah Jackson-Gwilt Alan Gall Teaching Science Christine Thompson Frog trade link to killer fungus Natural Environment Research Council Students to make ship history Arts & Humanities Research Council How parasites modify plants to attract insects Biotechnology & Biological Sciences Research Council Growing computers Engineering & Physical Sciences Research Council HIV study identifies key cellular defence mechanism Medical Research Council Physicists shed light on supernova mystery Science & Technology Facilities Council From the archives Alan Gall Journal puzzle solutions Alan Gall IST new members What is the IST? Cover images credits Front cover bottom left: Image courtesy of NASA Back cover top: Image courtesy of Wikipedia Commons Back cover middle: Image courtesy of NASA The Journal Page 1 Winter 2011 Editorial Welcome I hope that you enjoy this winter edition of the IST’s Journal. There are some really interesting and informative articles inside. -
Sanjay Limaye US Lead-Investigator Ludmila Zasova Russian Lead-Investigator Steering Committee K
Answer to the Call for a Medium-size mission opportunity in ESA’s Science Programme for a launch in 2022 (Cosmic Vision 2015-2025) EuropEan VEnus ExplorEr An in-situ mission to Venus Eric chassEfièrE EVE Principal Investigator IDES, Univ. Paris-Sud Orsay & CNRS Universite Paris-Sud, Orsay colin Wilson Co-Principal Investigator Dept Atm. Ocean. Planet. Phys. Oxford University, Oxford Takeshi imamura Japanese Lead-Investigator sanjay Limaye US Lead-Investigator LudmiLa Zasova Russian Lead-Investigator Steering Committee K. Aplin (UK) S. Lebonnois (France) K. Baines (USA) J. Leitner (Austria) T. Balint (USA) S. Limaye (USA) J. Blamont (France) J. Lopez-Moreno (Spain) E. Chassefière(F rance) B. Marty (France) C. Cochrane (UK) M. Moreira (France) Cs. Ferencz (Hungary) S. Pogrebenko (The Neth.) F. Ferri (Italy) A. Rodin (Russia) M. Gerasimov (Russia) J. Whiteway (Canada) T. Imamura (Japan) C. Wilson (UK) O. Korablev (Russia) L. Zasova (Russia) Sanjay Limaye Ludmilla Zasova Eric Chassefière Takeshi Imamura Colin Wilson University of IKI IDES ISAS/JAXA University of Oxford Wisconsin-Madison Laboratory of Planetary Space Science and Spectroscopy Univ. Paris-Sud Orsay & Engineering Center Space Research Institute CNRS 3-1-1, Yoshinodai, 1225 West Dayton Street Russian Academy of Sciences Universite Paris-Sud, Bat. 504. Sagamihara Dept of Physics Madison, Wisconsin, Profsoyusnaya 84/32 91405 ORSAY Cedex Kanagawa 229-8510 Parks Road 53706, USA Moscow 117997, Russia FRANCE Japan Oxford OX1 3PU Tel +1 608 262 9541 Tel +7-495-333-3466 Tel 33 1 69 15 67 48 Tel +81-42-759-8179 Tel 44 (0)1-865-272-086 Fax +1 608 235 4302 Fax +7-495-333-4455 Fax 33 1 69 15 49 11 Fax +81-42-759-8575 Fax 44 (0)1-865-272-923 [email protected] [email protected] [email protected] [email protected] [email protected] European Venus Explorer – Cosmic Vision 2015 – 2025 List of EVE Co-Investigators NAME AFFILIATION NAME AFFILIATION NAME AFFILIATION AUSTRIA Migliorini, A. -
USGS Open-File Report 2006-1263
Abstracts of the Annual Meeting of Planetary Geologic Mappers, Nampa, Idaho 2006 Edited By Tracy K.P. Gregg,1 Kenneth L. Tanaka,2 and R. Stephen Saunders3 Open-File Report 2006-1263 2006 Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. Government. U.S. DEPARTMENT OF THE INTERIOR U.S. GEOLOGICAL SURVEY 1 The State University of New York at Buffalo, Department of Geology, 710 Natural Sciences Complex, Buffalo, NY 14260-3050. 2 U.S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ 86001. 3 NASA Headquarters, Office of Space Science, 300 E. Street SW, Washington, DC 20546. Report of the Annual Mappers Meeting Northwest Nazarene University Nampa, Idaho June 30 – July 2, 2006 Approximately 18 people attended this year’s mappers meeting, and many more submitted abstracts and maps in absentia. The meeting was held on the campus of Northwest Nazarene University (NNU), and was graciously hosted by NNU’s School of Health and Science. Planetary mapper Dr. Jim Zimbelman is an alumnus of NNU, and he was pivotal in organizing the meeting at this location. Oral and poster presentations were given on Friday, June 30. Drs. Bill Bonnichsen and Marty Godchaux led field excursions on July 1 and 2. USGS Astrogeology Team Chief Scientist Lisa Gaddis led the meeting with a brief discussion of the status of the planetary mapping program at USGS, and a more detailed description of the Lunar Mapping Program. She indicated that there is now a functioning website (http://astrogeology.usgs.gov/Projects/PlanetaryMapping/Lunar/) which shows which lunar quadrangles are available to be mapped. -
Evidence for Crater Ejecta on Venus Tessera Terrain from Earth-Based Radar Images ⇑ Bruce A
Icarus 250 (2015) 123–130 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Evidence for crater ejecta on Venus tessera terrain from Earth-based radar images ⇑ Bruce A. Campbell a, , Donald B. Campbell b, Gareth A. Morgan a, Lynn M. Carter c, Michael C. Nolan d, John F. Chandler e a Smithsonian Institution, MRC 315, PO Box 37012, Washington, DC 20013-7012, United States b Cornell University, Department of Astronomy, Ithaca, NY 14853-6801, United States c NASA Goddard Space Flight Center, Mail Code 698, Greenbelt, MD 20771, United States d Arecibo Observatory, HC3 Box 53995, Arecibo 00612, Puerto Rico e Smithsonian Astrophysical Observatory, MS-63, 60 Garden St., Cambridge, MA 02138, United States article info abstract Article history: We combine Earth-based radar maps of Venus from the 1988 and 2012 inferior conjunctions, which had Received 12 June 2014 similar viewing geometries. Processing of both datasets with better image focusing and co-registration Revised 14 November 2014 techniques, and summing over multiple looks, yields maps with 1–2 km spatial resolution and improved Accepted 24 November 2014 signal to noise ratio, especially in the weaker same-sense circular (SC) polarization. The SC maps are Available online 5 December 2014 unique to Earth-based observations, and offer a different view of surface properties from orbital mapping using same-sense linear (HH or VV) polarization. Highland or tessera terrains on Venus, which may retain Keywords: a record of crustal differentiation and processes occurring prior to the loss of water, are of great interest Venus, surface for future spacecraft landings. -
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 -
1 Microwave Drilling: Introduction and Application Context 3
Microwave Drilling Final report Authors: S. Costanzo 1, G. Di Massa 1, A. Borgia 1, A. Raffo 1, T.W. Versloot 2, L. Summerer 2 Affiliation: 1DIMES – University of Calabria , 2Advanced Concepts Team, European Space Agency (ESA) Date: 31/05/2015 Contacts: Sandra Costanzo (Associate Professor) Tel: +39.0984.494652 Fax: +39.0984.494761 e-mail: [email protected] Leopold Summerer (Technical Officer) Tel: +31(0)715654192 Fax: +31(0)715658018 e-mail: [email protected] Ariadna ID: 14/9301 Ariadna study type: Standard Contract Number : 4000112047 Available on the ACT website http://www.esa.int/act Contents 1 Microwave Drilling: Introduction and Application Context 3 2 Microwave Bessel-Beam Launcher 6 2.1 BasicTheoryandDesignPrinciple . 6 2.2 X-BandBessel-BeamLauncher . 9 2.3 Experimental Validations of X-Band Bessel-Beam Launcher ............................... 11 3 DielectricEffectsofMicrowaveHeating 15 4 Bessel-Beam Launcher Application on Relevant Materials 18 4.1 Bessel-Beam Launcher Application on Basalt . 19 4.1.1 Experiments on 2 cm-Height Basalt: Dielectric Results . 20 4.1.2 Experiments on 6 cm-Height Basalt: Dielectric Results . 22 4.1.3 Experiments on 6 cm-Height Basalt: Thermal and Power Results ............................ 23 4.2 Bessel-Beam Launcher Application on Marble . 24 4.2.1 Experiments on Marble: Dielectric, Thermal and Power Results ............................ 24 5 MechanicalEffectsofBessel-Beam 30 6 ConclusionsandFutureDevelopments 32 2 1 Microwave Drilling: Introduction and Appli- cation Context The study of the subterranean composition of planets is an important tool for understanding the history and evolution of our solar system. By the analysis of burried soil samples it is possible to study materials exposed under past conditions and to investigate isotopic changes induced by interactions with the cosmic wind [1, 2, 3].