VENUS GRAVITY FIELD A. S. Kcmopliv and W. L

Total Page:16

File Type:pdf, Size:1020Kb

VENUS GRAVITY FIELD A. S. Kcmopliv and W. L , ., VENUS GRAVITY FIELD A. S. Kcmopliv and W. L. - Jet Propulsion Laboratory, California Institute of Technology, Pasadena; California 91109, U.S.A. A global gravity field model of Venus to degree and order 75 (5772 spherical harmonic coefficients) has been estimated from Doppler rad”io tracking of the orbiting spacecraft Pioneer Venus Orbiter (1979-1992) and Magellan (1990-1994). After the successful aerobraking of Magellan a near circular polar orbit was attained and relatively uniform gravity fieid resolution (= 200 km) was obtained with formal uncertainties of a few milligals. Detailed gravity for highland features such as E3eta Regio, Atla, Aphrodite Terra, Eisila Regio, Bell Regio and Ishtar Terra are displayed as gravity contours overlaying colored topography. The positive correlation of topography with gravity is very high being unlike that of the earth, moon and Mars. The amplitudes are earth like, but have significantly different gravity-topography ratios for different features (i.e., Atla and Beta have high ratios, whereas Aphrodite and lshtar have low ratios). The lowlands all display negative gravity anomalies and no mascon type features appear (i.e., gravity highs in circular basins). The largest negative anomaly is in Atalanta Planitia, the lowest elevation on Venus. The highest elevation on Venus is Maxwell Montes, however it does not have the largest gravity value. Both Theia Mons and Maat Mons have larger values. The smallest feature analyzed is the crater, Mead, which has a diameter of 280 km. H is essentially uncompensated, however the uncertainty in the modeling parameters allows a maximum of 300/. compensation. Global gravity, geoid and kiOSkitiC anomaly maps as well as the admittance function are displayed. 1. William L, Sjogren 2. PS-5 MS 301-150 Jet Propulsion Laboratory 3, Peter Janle California Institute of Technology 4800 Oak Grove Drive 4. None Pasadena, CA 91109, U.S.A. Phone: (818) 354-4868 5. Oral FAX: (818) 393-6388 e-mail [email protected]. gov 6. None.
Recommended publications
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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 .....................................................................................................................................
    [Show full text]
  • Volcanism and Tectonism in Rusalka Planitia and Atla Regio, Venus; M
    LPSC xn/ 767 VOLCANISM AND TECTONISM IN RUSALKA PLANITIA AND ATLA REGIO, VENUS; M. G. Lancaster and J. E. Guest (University of London Observatory, University College London, London, NW7 2QS, U. K.). In order to investigate the relationships between volcanism and tectonism in Rusalka Planitia and Atla Regio, the geology of four adjacent Cycle 1 Magellan ClMIDRs has been mapped (C100N180, C115N180, C115N197, and C100N197). These cover nearly 12 x 106 km2 between latitudes 7.6 S and 22.6 N, and longitudes 171.4 to 206.2 E. This region was chosen because it contains nearly all the types of volcanic and tectonic features observed on Venus, and covers plains as well as highlands. The western half of the region comprises most of the volcanic plains of Rusalka Planitia, which are characterized by a large-scale pervasive fabric of NW-SE trending sinuous ridges that resemble lunar and martian wrinkle ridges [I]. A NW-SE to N-S trending deformation belt occupies the SW comer of C100N180, and contains several coronae including Eigin Corona (5.0 S, 175.0 E). The belt is the source for large, radar-bright, plains forming, flood lava flow fields. A similar collection of corona-like centers and deformation belts composed largely of ridges, is found in the NE comer of C115N197, where an extensive collection of lava flow fields is also present. Other smaller regions of radar-bright lava lie scattered across the plains. A number of N-S to NNW-SSE trending ridge belts occupy the north-central part of these plains.
    [Show full text]
  • Venus Lithograph
    National Aeronautics and and Space Space Administration Administration 0 300,000,000 900,000,000 1,500,000,000 2,100,000,000 2,700,000,000 3,300,000,000 3,900,000,000 4,500,000,000 5,100,000,000 5,700,000,000 kilometers Venus www.nasa.gov Venus and Earth are similar in size, mass, density, composi- and at the surface are estimated to be just a few kilometers per SIGNIFICANT DATES tion, and gravity. There, however, the similarities end. Venus hour. How this atmospheric “super-rotation” forms and is main- 650 CE — Mayan astronomers make detailed observations of is covered by a thick, rapidly spinning atmosphere, creating a tained continues to be a topic of scientific investigation. Venus, leading to a highly accurate calendar. scorched world with temperatures hot enough to melt lead and Atmospheric lightning bursts, long suspected by scientists, were 1761–1769 — Two European expeditions to watch Venus cross surface pressure 90 times that of Earth (similar to the bottom confirmed in 2007 by the European Venus Express orbiter. On in front of the Sun lead to the first good estimate of the Sun’s of a swimming pool 1-1/2 miles deep). Because of its proximity Earth, Jupiter, and Saturn, lightning is associated with water distance from Earth. to Earth and the way its clouds reflect sunlight, Venus appears clouds, but on Venus, it is associated with sulfuric acid clouds. 1962 — NASA’s Mariner 2 reaches Venus and reveals the plan- to be the brightest planet in the sky. We cannot normally see et’s extreme surface temperatures.
    [Show full text]
  • Venera-D Landing Sites Selection and Cloud Layer Habitability Workshop Report
    1 Venera-D Landing Sites Selection and Cloud Layer Habitability Workshop Report IKI Moscow, Russia October 2-5, 2019 Space Science Research Institute (IKI), Russian Academy of Science, Roscosmos, and NASA http://venera-d.cosmos.ru/index.php?id=workshop2019&L=2 https://www.hou.usra.edu/meetings/venera-d2019/ 2 Table of Contents Introduction ...................................................................................................................................................... 6 Final Agenda .................................................................................................................................................. 10 Astrobiology Special Collection of papers from the workshop .................................................... 14 Technical Report: Venera-D Landing Site and Cloud Habitability Workshop ......................... 15 1.0 Missions to Venus .......................................................................................................................... 15 1.1 Past and Present ................................................................................................................................. 15 1.1.1 Available Instruments and Lessons Learned Surface Geology ........................................................... 15 1.1.2 Available Instruments and Lessons Learned for Cloud Habitability ............................................... 16 1.2 Future Missions ..................................................................................................................................
    [Show full text]
  • Surface Processes in the Venus Highlands: Results from Analysis of Magellan and a Recibo Data
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 104, NO. E], PAGES 1897-1916, JANUARY 25, 1999 Surface processes in the Venus highlands: Results from analysis of Magellan and A recibo data Bruce A. Campbell Center for Earth and Planetary Studies, Smithsonian Institution, Washington, D.C. Donald B. Campbell National Astronomy and Ionosphere Ceiitei-, Cornell University, Ithaca, New York Christopher H. DeVries Department of Physics and Astronomy, University of Massachusetts, Amherst Abstract. The highlands of Venus are characterized by an altitude-dependent change in radar backscattcr and microwave emissivity, likely produced by surface-atmosphere weathering re- actions. We analyzed Magellan and Arecibo data for these regions to study the roughness of the surface, lower radar-backscatter areas at the highest elevations, and possible causes for areas of anomalous behavior in Maxwell Montes. Arecibo data show that circular and linear radar polarization ratios rise with decreasing emissivity and increasing Fresnel reflectivity, supporting the hypothesis that surface scattering dominates the return from the highlands. The maximum values of these polarization ratios are consistent with a significant component of multiple-bounce scattering. We calibrated the Arecibo backscatter values using areas of overlap with Magellan coverage, and found that the echo at high incidence angles (up to 70") from the highlands is lower than expected for a predominantly diffuse scattering regime. This behavior may be due to geometric effects in multiple scattering from surface rocks, but fur- ther modeling is required. Areas of lower radar backscatter above an upper critical elevation are found to be generally consistent across the equatorial highlands, with the shift in micro- wave properties occurring over as little as 5ÜÜ m of elevation.
    [Show full text]
  • P5 11 Can Volcanoes Make Venus Habitable?
    Journal of Physics Special Topics An undergraduate physics journal P5 11 Can Volcanoes Make Venus Habitable? T. Cox, K. Penn Fernandez, L. Mead, J. Seagrave Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH December 17, 2020 Abstract This paper dives into the uses of converting Carbon dioxide (CO2) into Oxygen (O2). The aim of this paper is to examine if Venus' atmosphere could be terraformed to allow humans to breathe on the surface of the planet. What was found was that using power generated from 37 volcanoes known to be on Venus, it would take 186,666 MOXIE machines 1:38 × 1015 hours to convert Venus' atmosphere to 20% O2 Introduction chambers in volcanoes as a way to generate For this paper we will be using a MOXIE ma- electricity[6]. chine [1] (Mars Oxygen In-Situ Resource Utiliza- Finally, the assumptions that are being made tion Experiment), a machine that can convert for this paper are that the equipment needed to CO2 into O2. a MOXIE machine is designed convert Venus' atmosphere can easily be taken to for terraforming, it uses a reasonable amount of Venus, when breathing Venus' atmosphere there power of 300W to produce 10g per hour (as a are minimal harmful gases allowing this paper to maximum) of O2 [1]. ignore them and all volcanoes are similar to the Humans require an atmosphere minimum of Yellowstone volcano. The sole purpose of this 19.5% O2 to breathe [2], we will assume a mini- paper is to understand the possibility of turn- mum of 20% O2 in this paper.
    [Show full text]
  • BIGGEST VOLCANOES: a COMPARISON of IO and VENUS Betsy Mccall GLY 554, December 2-4, 2019 PROJECT OVERVIEW
    BIGGEST VOLCANOES: A COMPARISON OF IO AND VENUS Betsy McCall GLY 554, December 2-4, 2019 PROJECT OVERVIEW How do the largest volcanoes on Io and Venus differ? Io volcanic plume Maat Mons, Venus Source: http://www.seasky.org/solar- Source: system/assets/images/io03_sk12.jpg https://www.jpl.nasa.gov/spaceimages/details.php?id=PIA00106 MAAT MONS • Named for Egyptian goddess for truth and justice Ma’at • 395 km diameter • 8 km above mean planetary radius (5 km above surrounding plains) • May still be active • Source: https://encrypted- tbn0.gstatic.com/images?q=tbn%3AANd9GcSJVI h7OObuxOJRCZ8l2ka3gDEghJaz0FrAae0K88- HVJ6p36Vo GEOMORPHOLOGY & VOLCANOLOGY ▪ Found in a region of strong volcanic and tectonic activity ▪ At one end of Dali Chasma, thought to be a rifting process ▪ Possible ash flow on northern flank ▪ 1980s Pioneer Venus data could be explained by Plinian eruption on Source: Maat Mons https://d3i71xaburhd42.cloudfront.net/f15a9955baaa7b3773e4 be353172f1f23f013310/2-Figure1-1.png GEOMORPHOLOGY & VOLCANOLOGY • Different flow types on Maat Mons • Summit caldera of 31 km maximum diameter • Chain of small craters on southeast flank suggest collapse (lack of magma flows from craters) • No confirmation of recent activity Source: https://www.semanticscholar.org/paper/Geomorphology-and- volcanology-of-Maat-Mons%2C-Venus-Mouginis- Mark/f15a9955baaa7b3773e4be353172f1f23f013310/figure/6 WHAT IS THE LARGEST VOLCANO ON IO? • The answer to that question turns out to be murky • We’ll consider two possible candidates • Source: https://i.pinimg.com/736x/3a/81/51/3a8151d89
    [Show full text]
  • Automatic Creation of the Hypsometric Map of Venus
    AUTOMATIC CREATION OF THE HYPSOMETRIC MAP OF VENUS. E. N. Lazarev1, 2, J. F. Rodionova2. 1Moscow State University of Geodesy and Cartography, 4 Gorokhovskiy per., Moscow 105064, Russia, e-mail: [email protected], 2Sternberg State Astronomical Institute, 13 Universitetskiy pr., Moscow 119892, Russia, e-mail: [email protected] Introduction: The new hypsometric map of with the areas more than 10 000 sq. km at the Venus Venus is compiled at Sternberg State Astronomical surface, which corresponded with areas institute at a scale 1:45M. Detailed morphometric approximately more than 5 sq. km at the map. investigations of the planet were fulfilled too. At Contours in the areas of extreme values of heights this moment there are no more exact and (Maxwell Montes, Maat Mons, Teya Mons, Atalanta informative hypsometric maps of Earth group Planitia, Leda Planitia, Polar areas etc.) are showed planets hemispheres. The most of small-scale with exaggeration. general maps created by the last space researches Parallels and meridians of the Venus coordinate have been compiled in the cylindrical projections network are made every 20° of latitude and (mostly in Mercator projection) [1]. It can pick out longitude. The longitudes of Venus are measured the small-scale maps in «Atlas of the Earth Group from meridian of zero in the western direction from 0 Planets and their satellites» creating in MIIGAiK to 360°. The Venusian meridian of zero intersect [2]. The hypsometric map of Venus (1:45M) crater Ariadne in the North hemisphere. created under editing of Dr. Rodionova gives the The names of relief features are plotted at two representation of the planet relief on the basis of languages.
    [Show full text]
  • Geologic/Geomorphic Map of the Galindo Quadrangle (V-40), Venus
    U.S. DEPARTMENT OF THE INTERIOR TO ACCOMPANY MAP 1-2613 U.S. GEOLOGICAL SURVEY GEOLOGIC/GEOMORPHIC MAP OF THE GALINDO QUADRANGLE (V-40), VENUS By Mary G. Chapman INTRODUCTION plex area containing a mixture of different types of volcanic constructs, fracture zones, and plains. The map area, west The Galindo quadrangle (V-40; centered at lat 12.5° S., of Phoebe Regio, also contains a cluster of many sym­ long 255°) was geologically mapped at 1:5,000,000 scale metric, asymmetric, and multiple coronae, arachnoids, and under the Venus Data Analysis and Venus Geologic Map­ novae that appear to be randomly distributed (Stofan and ping Programs as part of a project focused on the study of others, 1992). Trending northeast across the east half of venusian geologic terrains containing assemblages of coro­ the map area is a tessera high that is the terminal end of nae, arachnoids, and novae; these are enigmatic circular a western arm of Phoebe Regio. The map area contains features perhaps related to hot-spot volcanism. Mapping of one of the deepest sections of Parga Chasma, a fractured the quadrangle indicates most coronae are related to exten­ depression that trends northwest across the south half of sion zones, and some aligned coronae and corona-like fea­ the map area. Parga Chasma varies greatly in depth (0 to 3 tures show systematic variations in age. km) and is approximately 1,870 km long, roughly connect­ Standard photogeologic techniques were used to map ing Themis Regio (southeast of the map area at about lat the geology on the synthetic aperture radar (SAR) backscat­ 35° S., long 285°) and Maat Mons (northwest of the map ter mosaic of V-40, which was generated by the radar­ area at about !at oo, long 195°).
    [Show full text]
  • Cosmoelements VENUS, an ACTIVE PLANET: EVIDENCE FOR
    CosmoELEMENTS VENUS, AN ACTIVE PLANET: EVIDENCE FOR RECENT VOLCANIC AND TECTONIC ACTIVITY Justin Filiberto1, Piero D’Incecco2,3, and Allan H. Treiman1 DOI: 10.2138/gselements.17.1.67 Similar in size to the Earth, Venus differs from our planet by its extreme surface temperature (470 °C), suffocating atmospheric pressure (about 92 times that of the Earth’s), and caustic atmosphere (mostly CO2, with sulfuric acid rain). Venus is Earth’s hellish twin sister. However, there are some similarities. As for the Earth, Venus has also had a very complex geologic history. During the early 1990s, NASA’s Magellan spacecraft imaged the surface of Venus with radar and gave us a panorama of a volcanic wonderland (Fig. 1). The surface of Venus is dotted with some of the largest volcanoes in the solar system, complete with summit calderas and extensive lava flows. Volcanoes on Venus resemble many of those on Earth, particularly those formed from the eruption of basaltic magma, such as Mauna Kea (Hawaii, USA) and Mount Etna (Italy). One of the biggest unresolved scientific questions about Venus concerns its style and rate of volcanism during its geologic past. Did volcanic eruptions on Color overlay of heat patterns from Idunn Mons and Imdr Regio as FIGURE 2 Venus occur locally and constantly in time? Or did the planet undergo derived from VIRTIS (visible and infrared thermal imaging spectrom- eter) surface brightness data overlain on Magellan radar data as in Figure 1. Red sporadic events of global and catastrophic volcanism which rejuvenated represents the warmest regions (emissivity ≥0.9), interpreted to be the freshest its entire crust in a short amount of time? basalts, while the blue/purple are cooler regions (emissivity ~0.5), interpreted to be altered older basalts.
    [Show full text]