First Gravity Traverse on the Martian Surface from the Curiosity Rover
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Interpretations of Gravity Anomalies at Olympus Mons, Mars: Intrusions, Impact Basins, and Troughs
Lunar and Planetary Science XXXIII (2002) 2024.pdf INTERPRETATIONS OF GRAVITY ANOMALIES AT OLYMPUS MONS, MARS: INTRUSIONS, IMPACT BASINS, AND TROUGHS. P. J. McGovern, Lunar and Planetary Institute, Houston TX 77058-1113, USA, ([email protected]). Summary. New high-resolution gravity and topography We model the response of the lithosphere to topographic loads data from the Mars Global Surveyor (MGS) mission allow a re- via a thin spherical-shell flexure formulation [9, 12], obtain- ¡g examination of compensation and subsurface structure models ing a model Bouguer gravity anomaly ( bÑ ). The resid- ¡g ¡g ¡g bÓ bÑ in the vicinity of Olympus Mons. ual Bouguer anomaly bÖ (equal to - ) can be Introduction. Olympus Mons is a shield volcano of enor- mapped to topographic relief on a subsurface density interface, using a downward-continuation filter [11]. To account for the mous height (> 20 km) and lateral extent (600-800 km), lo- cated northwest of the Tharsis rise. A scarp with height up presence of a buried basin, we expand the topography of a hole Ö h h ¼ ¼ to 10 km defines the base of the edifice. Lobes of material with radius and depth into spherical harmonics iÐÑ up h with blocky to lineated morphology surround the edifice [1-2]. to degree and order 60. We treat iÐÑ as the initial surface re- Such deposits, known as the Olympus Mons aureole deposits lief, which is compensated by initial relief on the crust mantle =´ µh c Ñ c (hereinafter abbreviated as OMAD), are of greatest extent to boundary of magnitude iÐÑ . These interfaces the north and west of the edifice. -
Preliminary Estimation and Validation of Polar Motion Excitation from Different Types of the GRACE and GRACE Follow-On Missions Data
remote sensing Article Preliminary Estimation and Validation of Polar Motion Excitation from Different Types of the GRACE and GRACE Follow-On Missions Data Justyna Sliwi´ ´nska 1,* , Małgorzata Wi ´nska 2 and Jolanta Nastula 1 1 Space Research Centre, Polish Academy of Sciences, 00-716 Warsaw, Poland; [email protected] 2 Faculty of Civil Engineering, Warsaw University of Technology, 00-637 Warsaw, Poland; [email protected] * Correspondence: [email protected] Received: 18 September 2020; Accepted: 22 October 2020; Published: 23 October 2020 Abstract: The Gravity Recovery and Climate Experiment (GRACE) mission has provided global observations of temporal variations in the gravity field resulting from mass redistribution at the surface and within the Earth for the period 2002–2017. Although GRACE satellites are not able to realistically detect the second zonal parameter (DC20) of geopotential associated with the flattening of the Earth, they can accurately determine variations in degree-2 order-1 (DC21, DS21) coefficients that are proportional to variations in polar motion. Therefore, GRACE measurements are commonly exploited to interpret polar motion changes due to variations in the global mass redistribution, especially in the continental hydrosphere and cryosphere. Such impacts are usually examined by computing the so-called hydrological polar motion excitation (HAM) and cryospheric polar motion excitation (CAM), often analyzed together as HAM/CAM. The great success of the GRACE mission and the scientific robustness of its data contributed to the launch of its successor, GRACE Follow-On (GRACE-FO), which began in May 2018 and continues to the present. This study presents the first estimates of HAM/CAM computed from GRACE-FO data provided by three data centers: Center for Space Research (CSR), Jet Propulsion Laboratory (JPL), and GeoForschungsZentrum (GFZ). -
No. 40. the System of Lunar Craters, Quadrant Ii Alice P
NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates. -
Appendix a Conceptual Geologic Model
Newberry Geothermal Energy Establishment of the Frontier Observatory for Research in Geothermal Energy (FORGE) at Newberry Volcano, Oregon Appendix A Conceptual Geologic Model April 27, 2016 Contents A.1 Summary ........................................................................................................................................... A.1 A.2 Geological and Geophysical Context of the Western Flank of Newberry Volcano ......................... A.2 A.2.1 Data Sources ...................................................................................................................... A.2 A.2.2 Geography .......................................................................................................................... A.3 A.2.3 Regional Setting ................................................................................................................. A.4 A.2.4 Regional Stress Orientation .............................................................................................. A.10 A.2.5 Faulting Expressions ........................................................................................................ A.11 A.2.6 Geomorphology ............................................................................................................... A.12 A.2.7 Regional Hydrology ......................................................................................................... A.20 A.2.8 Natural Seismicity ........................................................................................................... -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
Detection of Caves by Gravimetry
Detection of Caves by Gravimetry By HAnlUi'DO J. Cmco1) lVi/h plates 18 (1)-21 (4) Illtroduction A growing interest in locating caves - largely among non-speleolo- gists - has developed within the last decade, arising from industrial or military needs, such as: (1) analyzing subsUl'face characteristics for building sites or highway projects in karst areas; (2) locating shallow caves under airport runways constructed on karst terrain covered by a thin residual soil; and (3) finding strategic shelters of tactical significance. As a result, geologists and geophysicists have been experimenting with the possibility of applying standard geophysical methods toward void detection at shallow depths. Pioneering work along this line was accomplishecl by the U.S. Geological Survey illilitary Geology teams dUl'ing World War II on Okinawan airfields. Nicol (1951) reported that the residual soil covel' of these runways frequently indicated subsi- dence due to the collapse of the rooves of caves in an underlying coralline-limestone formation (partially detected by seismic methods). In spite of the wide application of geophysics to exploration, not much has been published regarding subsUl'face interpretation of ground conditions within the upper 50 feet of the earth's surface. Recently, however, Homberg (1962) and Colley (1962) did report some encoUl'ag- ing data using the gravity technique for void detection. This led to the present field study into the practical means of how this complex method can be simplified, and to a use-and-limitations appraisal of gravimetric techniques for speleologic research. Principles all(1 Correctiolls The fundamentals of gravimetry are based on the fact that natUl'al 01' artificial voids within the earth's sUl'face - which are filled with ail' 3 (negligible density) 01' water (density about 1 gmjcm ) - have a remark- able density contrast with the sUl'roun<ling rocks (density 2.0 to 1) 4609 Keswick Hoad, Baltimore 10, Maryland, U.S.A. -
Airborne Geoid Determination
LETTER Earth Planets Space, 52, 863–866, 2000 Airborne geoid determination R. Forsberg1, A. Olesen1, L. Bastos2, A. Gidskehaug3,U.Meyer4∗, and L. Timmen5 1KMS, Geodynamics Department, Rentemestervej 8, 2400 Copenhagen NV, Denmark 2Astronomical Observatory, University of Porto, Portugal 3Institute of Solid Earth Physics, University of Bergen, Norway 4Alfred Wegener Institute, Bremerhaven, Germany 5Geo Forschungs Zentrum, Potsdam, Germany (Received January 17, 2000; Revised August 18, 2000; Accepted August 18, 2000) Airborne geoid mapping techniques may provide the opportunity to improve the geoid over vast areas of the Earth, such as polar areas, tropical jungles and mountainous areas, and provide an accurate “seam-less” geoid model across most coastal regions. Determination of the geoid by airborne methods relies on the development of airborne gravimetry, which in turn is dependent on developments in kinematic GPS. Routine accuracy of airborne gravimetry are now at the 2 mGal level, which may translate into 5–10 cm geoid accuracy on regional scales. The error behaviour of airborne gravimetry is well-suited for geoid determination, with high-frequency survey and downward continuation noise being offset by the low-pass gravity to geoid filtering operation. In the paper the basic principles of airborne geoid determination are outlined, and examples of results of recent airborne gravity and geoid surveys in the North Sea and Greenland are given. 1. Introduction the sea-surface (H) by airborne altimetry. This allows— Precise geoid determination has in recent years been facil- in principle—the determination of the dynamic sea-surface itated through the progress in airborne gravimetry. The first topography (ζ) through the equation large-scale aerogravity experiment was the airborne gravity survey of Greenland 1991–92 (Brozena, 1991). -
Arxiv:2003.06799V2 [Astro-Ph.EP] 6 Feb 2021
Thomas Ruedas1,2 Doris Breuer2 Electrical and seismological structure of the martian mantle and the detectability of impact-generated anomalies final version 18 September 2020 published: Icarus 358, 114176 (2021) 1Museum für Naturkunde Berlin, Germany 2Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany arXiv:2003.06799v2 [astro-ph.EP] 6 Feb 2021 The version of record is available at http://dx.doi.org/10.1016/j.icarus.2020.114176. This author pre-print version is shared under the Creative Commons Attribution Non-Commercial No Derivatives License (CC BY-NC-ND 4.0). Electrical and seismological structure of the martian mantle and the detectability of impact-generated anomalies Thomas Ruedas∗ Museum für Naturkunde Berlin, Germany Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany Doris Breuer Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany Highlights • Geophysical subsurface impact signatures are detectable under favorable conditions. • A combination of several methods will be necessary for basin identification. • Electromagnetic methods are most promising for investigating water concentrations. • Signatures hold information about impact melt dynamics. Mars, interior; Impact processes Abstract We derive synthetic electrical conductivity, seismic velocity, and density distributions from the results of martian mantle convection models affected by basin-forming meteorite impacts. The electrical conductivity features an intermediate minimum in the strongly depleted topmost mantle, sandwiched between higher conductivities in the lower crust and a smooth increase toward almost constant high values at depths greater than 400 km. The bulk sound speed increases mostly smoothly throughout the mantle, with only one marked change at the appearance of β-olivine near 1100 km depth. -
Shape of the Northern Hemisphere of Mars from the Mars Orbiter Laser Altimeter (MOLA)
GEOPHYSICAL RESEARCH LETTERS, VOL. 25, NO. 24, PAGES 4393-4396, DECEMBER 15, 1998 Shape of the northern hemisphere of Mars from the Mars Orbiter Laser Altimeter (MOLA) Maria T. Zuber1,2, David E. Smith2, Roger J. Phillips3, Sean C. Solomon4, W. Bruce Banerdt5,GregoryA.Neumann1,2, Oded Aharonson1 Abstract. Eighteen profiles of ∼N-S-trending topography potentially change the flattening by at most 5%. Allowing from the Mars Orbiter Laser Altimeter (MOLA) are used for the 3.1-km offset of the center of mass (COM) from the to analyze the shape of Mars’ northern hemisphere. MOLA center of figure (COF) along the polar axis [Smith and Zuber, observations show smaller northern hemisphere flattening 1996], we can expect the flattening of the full planet to be than previously thought. The hypsometric distribution is less than that of the northern hemisphere by ∼ 15%, or narrowly peaked with > 20% of the surface lying within 200 1/174 6. This is significantly less than the earlier value m of the mean elevation. Low elevation correlates with low of 1/154.4[Bills and Ferrari, 1978] and slightly less than surface roughness, but the elevation and roughness may re- the ellipsoidal value of 1/166.53 [Smith and Zuber, 1996] flect different mechanisms. Bouguer gravity indicates less that have been used in geophysical analyses. However, it variability in crustal thickness and/or lateral density struc- is larger than the flattening of 1/192 used in making maps ture than previously expected. The 3.1-km offset between [Wu, 1991]. Consideration of ice cap topography will further centers of mass and figure along the polar axis results in a decrease the value. -
Resolving Geophysical Signals by Terrestrial Gravimetry: a Time Domain Assessment of the Correction-Induced Uncertainty
Originally published as: Mikolaj, M., Reich, M., Güntner, A. (2019): Resolving Geophysical Signals by Terrestrial Gravimetry: A Time Domain Assessment of the Correction-Induced Uncertainty. - Journal of Geophysical Research, 124, 2, pp. 2153—2165. DOI: http://doi.org/10.1029/2018JB016682 RESEARCH ARTICLE Resolving Geophysical Signals by Terrestrial Gravimetry: 10.1029/2018JB016682 A Time Domain Assessment of the Correction-Induced Key Points: Uncertainty • Global-scale uncertainty assessment of tidal, oceanic, large-scale 1 1 1,2 hydrological, and atmospheric M. Mikolaj , M. Reich , and A. Güntner corrections for terrestrial gravimetry • Resolving subtle gravity signals in the 1Section Hydrology, GFZ German Research Centre for Geosciences, Potsdam, Germany, 2Institute of Environmental order of few nanometers per square Science and Geography, University of Potsdam, Potsdam, Germany second is challenged by the statistical uncertainty of correction models • Uncertainty computed for selected periods varies significantly Abstract Terrestrial gravimetry is increasingly used to monitor mass transport processes in with latitude and altitude of the geophysics boosted by the ongoing technological development of instruments. Resolving a particular gravimeter phenomenon of interest, however, requires a set of gravity corrections of which the uncertainties have not been addressed up to now. In this study, we quantify the time domain uncertainty of tide, global Supporting Information: atmospheric, large-scale hydrological, and nontidal ocean loading corrections. The uncertainty is • Supporting Information S1 assessed by comparing the majority of available global models for a suite of sites worldwide. The average uncertainty expressed as root-mean-square error equals 5.1 nm/s2, discounting local hydrology or air Correspondence to: pressure. The correction-induced uncertainty of gravity changes over various time periods of interest M. -
Pre-Mission Insights on the Interior of Mars Suzanne E
Pre-mission InSights on the Interior of Mars Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, Ulrich Christensen, Véronique Dehant, Mélanie Drilleau, William Folkner, Nobuaki Fuji, et al. To cite this version: Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, et al.. Pre-mission InSights on the Interior of Mars. Space Science Reviews, Springer Verlag, 2019, 215 (1), pp.1-72. 10.1007/s11214-018-0563-9. hal-01990798 HAL Id: hal-01990798 https://hal.archives-ouvertes.fr/hal-01990798 Submitted on 23 Jan 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Open Archive Toulouse Archive Ouverte (OATAO ) OATAO is an open access repository that collects the wor of some Toulouse researchers and ma es it freely available over the web where possible. This is an author's version published in: https://oatao.univ-toulouse.fr/21690 Official URL : https://doi.org/10.1007/s11214-018-0563-9 To cite this version : Smrekar, Suzanne E. and Lognonné, Philippe and Spohn, Tilman ,... [et al.]. Pre-mission InSights on the Interior of Mars. (2019) Space Science Reviews, 215 (1). -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei