Present True Polar Wander in the Frame of the Geotectonic Reference System
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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). -
Long-Term Rotational Effects on the Shape of the Earth and Its Oceans
LONG-TERM ROTATIONAL EFFECTS ON THE SHAPE OF THE EARTH AND ITS OCEANS Jonathan Edwin Mound A thesis submitted in cooforrnity with the reqnhents for the degree of Doctor of Philosophy Gradiiate Depart ment of P hysics University of Toront O @ Copyright by Jonathan E. Mound 2001 . .. ilbitionsand et 9-Bib iogrephic SeMces -Iiographiques 395 WeIlington Street 395, ni6 Wellington ûttawa ON K1AOW OtEaweON KtAW Canada Canada The author has granted a non- L'auteur a accorde une licence ncm exdusive licence allouing the exclusive permettant à la National Library of Cana& to Bibliotheque natiode du Canada de reproduce, Ioan, distriibute or seli reproduire, prêter, distniuer ou copies of this thesis in microform, vendre des copies de cette thèse sous paper or electronic formats. la forme de microfiche/film, de reprociucbon sur papier ou sur format électronique. The author retains ownership of the L'auteur conserve la propriété du copyright in this thesis. Neither the droit d'auteur qui protège cette thèse. ttiesis nor substantial extracts &om it Ni la thèse ni des extraits substantiels may be printed or otherwise de celle-ci ne doivent être imprimés reproduced without the author's ou autrement reproduits sans son permission. autorisation. LONG-TERM RQTATLONAL E-FFECTS ON THE SHAPE OF THE EARTH AND ITS OCEANS Doctor of Philosophy, 2001. Jonathan E. Mound Department of Physics, University of Toronto Abstract The centrifuga1 potent ial associated with the Eart h's rotation influences the shape of both the solid Earth and the oceaos. Changes in rotation t hus deform both the ocean and solid surfaces. -
Testing the Axial Dipole Hypothesis for the Moon by Modeling the Direction of Crustal Magnetization J
Testing the axial dipole hypothesis for the Moon by modeling the direction of crustal magnetization J. Oliveira, M. Wieczorek To cite this version: J. Oliveira, M. Wieczorek. Testing the axial dipole hypothesis for the Moon by modeling the direction of crustal magnetization. Journal of Geophysical Research. Planets, Wiley-Blackwell, 2017, 122 (2), pp.383-399. 10.1002/2016JE005199. hal-02105528 HAL Id: hal-02105528 https://hal.archives-ouvertes.fr/hal-02105528 Submitted on 21 Apr 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. Journal of Geophysical Research: Planets RESEARCH ARTICLE Testing the axial dipole hypothesis for the Moon by modeling 10.1002/2016JE005199 the direction of crustal magnetization Key Points: • The direction of magnetization within J. S. Oliveira1 and M. A. Wieczorek1,2 the lunar crust was inverted using a unidirectional magnetization model 1Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris Diderot, CNRS, Paris, France, 2Université Côte • The paleomagnetic poles of several d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France isolated anomalies are not randomly distributed, and some have equatorial latitudes • The distribution of paleopoles may Abstract Orbital magnetic field data show that portions of the Moon’s crust are strongly magnetized, be explained by a dipolar magnetic and paleomagnetic data of lunar samples suggest that Earth strength magnetic fields could have existed field that was not aligned with the during the first several hundred million years of lunar history. -
True Polar Wander of Mercury
Mercury: Current and Future Science 2018 (LPI Contrib. No. 2047) 6098.pdf TRUE POLAR WANDER OF MERCURY. J. T. Keane1 and I. Matsuyama2; 1California Institute of Technology, Pasadena, CA 91125, USA ([email protected]); 2Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. Introduction: The spin of a planet is not constant to the Sun and subject to stronger tidal and rotational with time. Planetary spins evolve on a variety of time- forces. However, even with this corrected dynamical scales due to a variety of internal and external forces. oblateness, the required orbital configuration appears One process for changing the spin of a planet is true po- unreasonable−requiring semimajor axes <0.1 AU [5]. lar wander (TPW). TPW is the reorientation of the bulk An alternative explanation may be that a large fraction planet with respect to inertial space due to the redistri- of Mercury’s figure is a “thermal” figure, set Mercury’s bution of mass on or within the planet. The redistribu- close proximity to the Sun and its unique spin-orbit res- tion of mass alters the planet’s moments of inertia onance [7-8] (which are related to the planet’s spherical harmonic de- True Polar Wander of Mercury: While Mercury’s gree/order-2 gravity field). This process has been meas- impact basins and volcanic provinces cannot explain ured on the Earth, and inferred for a variety of solar sys- Mercury’s anomalous figure, they still have an im- tem bodies [1]. TPW can have significant consequences portant effect on planet’s moments of inertia and orien- for the climate, tectonics, and geophysics of a planet. -
True Polar Wander: Linking Deep and Shallow Geodynamics to Hydro- and Bio-Spheric Hypotheses T
True Polar Wander: linking Deep and Shallow Geodynamics to Hydro- and Bio-Spheric Hypotheses T. D. Raub, Yale University, New Haven, CT, USA J. L. Kirschvink, California Institute of Technology, Pasadena, CA, USA D. A. D. Evans, Yale University, New Haven, CT, USA © 2007 Elsevier SV. All rights reserved. 5.14.1 Planetary Moment of Inertia and the Spin-Axis 565 5.14.2 Apparent Polar Wander (APW) = Plate motion +TPW 566 5.14.2.1 Different Information in Different Reference Frames 566 5.14.2.2 Type 0' TPW: Mass Redistribution at Clock to Millenial Timescales, of Inconsistent Sense 567 5.14.2.3 Type I TPW: Slow/Prolonged TPW 567 5.14.2.4 Type II TPW: Fast/Multiple/Oscillatory TPW: A Distinct Flavor of Inertial Interchange 569 5.14.2.5 Hypothesized Rapid or Prolonged TPW: Late Paleozoic-Mesozoic 569 5.14.2.6 Hypothesized Rapid or Prolonged TPW: 'Cryogenian'-Ediacaran-Cambrian-Early Paleozoic 571 5.14.2.7 Hypothesized Rapid or Prolonged TPW: Archean to Mesoproterozoic 572 5.14.3 Geodynamic and Geologic Effects and Inferences 572 5.14.3.1 Precision of TPW Magnitude and Rate Estimation 572 5.14.3.2 Physical Oceanographic Effects: Sea Level and Circulation 574 5.14.3.3 Chemical Oceanographic Effects: Carbon Oxidation and Burial 576 5..14.4 Critical Testing of Cryogenian-Cambrian TPW 579 5.14A1 Ediacaran-Cambrian TPW: 'Spinner Diagrams' in the TPW Reference Frame 579 5.14.4.2 Proof of Concept: Independent Reconstruction of Gondwanaland Using Spinner Diagrams 581 5.14.5 Summary: Major Unresolved Issues and Future Work 585 References 586 5.14.1 Planetary Moment of Inertia location ofEarth's daily rotation axis and/or by fluc and the Spin-Axis tuations in the spin rate ('length of day' anomalies). -
Earth Orientation Parameters from VLBI Determined with a Kalman Filter
Originally published as: Karbon, M., Soja, B., Nilsson, T., Deng, Z., Heinkelmann, R., Schuh, H. (2017): Earth orientation parameters from VLBI determined with a Kalman filter. ‐ Geodesy and Geodynamics, 8, 6, pp. 396— 407. DOI: http://doi.org/10.1016/j.geog.2017.05.006 Geodesy and Geodynamics 8 (2017) 396e407 Contents lists available at ScienceDirect Geodesy and Geodynamics journal homepages: www.keaipublishing.com/en/journals/geog; http://www.jgg09.com/jweb_ddcl_en/EN/volumn/home.shtml Earth orientation parameters from VLBI determined with a Kalman filter * Maria Karbon a, , Benedikt Soja b, Tobias Nilsson a, Zhiguo Deng a, Robert Heinkelmann a, Harald Schuh a, c a GFZ German Research Centre for Geosciences, Telegrafenberg A17, Potsdam, Germany b Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA c Technical University of Berlin, Strabe des 17. Juni 135, Berlin, Germany article info abstract Article history: This paper introduces the reader to our Kalman filter developed for geodetic VLBI (very long baseline Received 24 November 2016 interferometry) data analysis. The focus lies on the EOP (Earth Orientation Parameter) determination Received in revised form based on the Continuous VLBI Campaign 2014 (CONT14) data, but also earlier CONT campaigns are 23 May 2017 analyzed. For validation and comparison purposes we use EOP determined with the classical LSM Accepted 24 May 2017 (least squares method) estimated from the same VLBI data set as the Kalman solution with a daily Available online 6 September 2017 resolution. To gain higher resolved EOP from LSM we run solutions which yield hourly estimates for polar motion and dUT1 ¼ Universal Time (UT1) e Coordinated Universal Time (UTC). -
A Novel Plate Tectonic Scenario for the Genesis and Sealing of Some Major Mesozoic Oil Fields
It’s Time—Renew Your GSA Membership and Save 15% DECEMBER | VOL. 26, 2016 12 NO. A PUBLICATION OF THE GEOLOGICAL SOCIETY OF AMERICA® IRAQ A Novel Plate Tectonic Scenario for the Genesis KUWAIT and Sealing of Some Major PERSIAN GULF Mesozoic Oil Fields IRAN BAHRAIN Ghawar Field QATAR SAUDI ARABIA OMAN U.A.E. DECEMBER 2016 | VOLUME 26, NUMBER 12 GSA TODAY (ISSN 1052-5173 USPS 0456-530) prints news Featured Articles and information for more than 26,000 GSA member readers and subscribing libraries, with 11 monthly issues (March/ April is a combined issue). GSA TODAY is published by The Geological Society of America® Inc. (GSA) with offices at SCIENCE 3300 Penrose Place, Boulder, Colorado, USA, and a mail- ing address of P.O. Box 9140, Boulder, CO 80301-9140, USA. 4 A Novel Plate Tectonic Scenario for the Genesis GSA provides this and other forums for the presentation and Sealing of Some Major Mesozoic Oil Fields of diverse opinions and positions by scientists worldwide, Giovanni Muttoni and Dennis V. Kent regardless of race, citizenship, gender, sexual orientation, religion, or political viewpoint. Opinions presented in this Cover: NASA satellite photo of the Persian Gulf area publication do not reflect official positions of the Society. with the Ghawar Oil Field in the lower left of the picture. © 2016 The Geological Society of America Inc. All rights See related article, p. 4–10. reserved. Copyright not claimed on content prepared wholly by U.S. government employees within the scope of their employment. Individual scientists are hereby granted permission, without fees or request to GSA, to use a single GROUNDWORK figure, table, and/or brief paragraph of text in subsequent work and to make/print unlimited copies of items in GSA 36 Physical Experiments of Tectonic Deformation TODAY for noncommercial use in classrooms to further and Processes: Building a Strong Community education and science. -
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Contents lists available at ScienceDirect Palaeogeography, Palaeoclimatology, Palaeoecology journal homepage: www.elsevier.com/locate/palaeo Pangea B and the Late Paleozoic Ice Age ⁎ D.V. Kenta,b, ,G.Muttonic a Earth and Planetary Sciences, Rutgers University, Piscataway, NJ 08854, USA b Lamont-Doherty Earth Observatory of Columbia University, Palisades, NY 10964, USA c Dipartimento di Scienze della Terra 'Ardito Desio', Università degli Studi di Milano, via Mangiagalli 34, I-20133 Milan, Italy ARTICLE INFO ABSTRACT Editor: Thomas Algeo The Late Paleozoic Ice Age (LPIA) was the penultimate major glaciation of the Phanerozoic. Published compi- Keywords: lations indicate it occurred in two main phases, one centered in the Late Carboniferous (~315 Ma) and the other Late Paleozoic Ice Age in the Early Permian (~295 Ma), before waning over the rest of the Early Permian and into the Middle Permian Pangea A (~290 Ma to 275 Ma), and culminating with the final demise of Alpine-style ice sheets in eastern Australia in the Pangea B Late Permian (~260 to 255 Ma). Recent global climate modeling has drawn attention to silicate weathering CO2 Greater Variscan orogen consumption of an initially high Greater Variscan edifice residing within a static Pangea A configuration as the Equatorial humid belt leading cause of reduction of atmospheric CO2 concentrations below glaciation thresholds. Here we show that Silicate weathering CO2 consumption the best available and least-biased paleomagnetic reference poles place the collision between Laurasia and Organic carbon burial Gondwana that produced the Greater Variscan orogen in a more dynamic position within a Pangea B config- uration that had about 30% more continental area in the prime equatorial humid belt for weathering and which drifted northward into the tropical arid belt as it transformed to Pangea A by the Late Permian. -
Apparent and True Polar Wander and the Geometry of the Geomagnetic
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. B11, 2300, doi:10.1029/2000JB000050, 2002 Correction published 10 October 2003 Apparent and true polar wander and the geometry of the geomagnetic field over the last 200 Myr Jean Besse and Vincent Courtillot Laboratoire de Pale´omagne´tisme, UMR 7577, Institut de Physique du Globe de Paris, Paris, France Received 8 November 2000; revised 15 January 2002; accepted 20 January 2002; published 15 November 2002. [1] We have constructed new apparent polar wander paths (APWPs) for major plates over the last 200 Myr. Updated kinematic models and selected paleomagnetic data allowed us to construct a master APWP. A persistent quadrupole moment on the order of 3% of the dipole over the last 200 Myr is suggested. Paleomagnetic and hot spot APW are compared, and a new determination of ‘‘true polar wander’’ (TPW) is derived. Under the hypothesis of fixed Atlantic and Indian hot spots, we confirm that TPW is episodic, with periods of (quasi) standstill alternating with periods of faster TPW (in the Cretaceous). The typical duration of these periods is on the order of a few tens of millions of years with wander rates during fast tracks on the order of 30 to 50 km/Myr. A total TPW of some 30° is suggested for the last 200 Myr. We find no convincing evidence for episodes of superfast TPW such as proposed recently by a number of authors. Comparison over the last 130 Myr of TPW deduced from hot spot tracks and paleomagnetic data in the Indo-Atlantic hemisphere with an independent determination for the Pacific plate supports the idea that, to first order, TPW is a truly global feature of Earth dynamics. -
True Polar Wander Recorded by the Distribution of Martian Valley Networks S
46th Lunar and Planetary Science Conference (2015) 1887.pdf TRUE POLAR WANDER RECORDED BY THE DISTRIBUTION OF MARTIAN VALLEY NETWORKS S. Bouley1 , D. Baratoux2, I. Matsuyama3, F. Forget4, F. Costard1 and A. Séjourné,1 - 1GEOPS – UMR 8148- Bât.509, Université Paris Sud - 91405 Orsay Cedex ([email protected]), 2 Geosciences Environnement Toulouse, Université de Toulouse III UMR 5563, 14 Avenue Edouard Belin, 31400, Toulouse, France, 3Lunar and Planetary Laboratory, University of Arizona, AZ, USA, 4Laboratoire de Métérologie Dynamique, Institut Pierre Simon Laplace, Paris, France Introduction: Hesperian-Noachian (older than 3.5 putative paleoshorelines of the northern ocean [7]. Ga) Martian valley networks (VNs) are essentially However, the latter hypothesis was not confirmed by located on the highlands [1,2,3] within a domain of the elevations of deltas [13]. Once again, the position latitudes ranging from – 60°S to +30°N and are con- of the paleopoles inferred from the VNs distribution is sidered to be one of the best evidences for different consistent with TPW driven by the formation of Thar- climatic conditions during early Mars [e.g., 4,5]. In this sis. Estimates of the paleopole location prior to the study, we show that their distribution suggest a reori- formation of Tharsis using gravity data are consistent entation of Mars’ rotation axis with respect to the man- with the paleopoles found in this study (95°W, 65°N, tle, or true polar wander (TPW) . The timing and char- [6], 100.5 ± 49.5°E, 71.1+17.5°N [10]). The paleo acteristics of this true polar wander event appear to be south-pole (62°E, 69°S) is also close to the center of also supported by other independent observations. -
Constraining Ceres' Interior from Its Rotational Motion
A&A 535, A43 (2011) Astronomy DOI: 10.1051/0004-6361/201116563 & c ESO 2011 Astrophysics Constraining Ceres’ interior from its rotational motion N. Rambaux1,2, J. Castillo-Rogez3, V. Dehant4, and P. Kuchynka2,3 1 Université Pierre et Marie Curie, UPMC–Paris 06, France e-mail: [nicolas.rambaux;kuchynka]@imcce.fr 2 IMCCE, Observatoire de Paris, CNRS UMR 8028, 77 avenue Denfert-Rochereau, 75014 Paris, France 3 Jet Propulsion Laboratory, Caltech, Pasadena, USA e-mail: [email protected] 4 Royal Observatory of Belgium, 3 avenue Circulaire, 1180 Brussels, Belgium Received 24 January 2011 / Accepted 14 July 2011 ABSTRACT Context. Ceres is the most massive body of the asteroid belt and contains about 25 wt.% (weight percent) of water. Understanding its thermal evolution and assessing its current state are major goals of the Dawn mission. Constraints on its internal structure can be inferred from various types of observations. In particular, detailed knowledge of the rotational motion can help constrain the mass distribution inside the body, which in turn can lead to information about its geophysical history. Aims. We investigate the signature of internal processes on Ceres rotational motion and discuss future measurements that can possibly be performed by the spacecraft Dawn and will help to constrain Ceres’ internal structure. Methods. We compute the polar motion, precession-nutation, and length-of-day variations. We estimate the amplitudes of the rigid and non-rigid responses for these various motions for models of Ceres’ interior constrained by shape data and surface properties. Results. As a general result, the amplitudes of oscillations in the rotation appear to be small, and their determination from spaceborne techniques will be challenging. -
Mantle Anchor Structure: an Argument for Bottom up Tectonics
Earth and Planetary Science Letters 299 (2010) 69–79 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl Mantle Anchor Structure: An argument for bottom up tectonics Adam M. Dziewonski a,⁎, Vedran Lekic b,1, Barbara A. Romanowicz b a Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA, USA b Berkeley Seismological Laboratory, University of California, Berkeley, CA, USA article info abstract Article history: Close examination of the long wavelength shear velocity signal in the lowermost mantle in the wavenumber Received 25 January 2010 domain ties several geophysical observations together and leads to fundamental inferences. When mantle Received in revised form 2 August 2010 shear velocity model S362ANI at a depth of 2800 km is expanded in spherical harmonics up to degree 18, Accepted 6 August 2010 more than one half of the seismic model's total power is contained in a single spherical harmonic coefficient: Available online 28 September 2010 the “recumbent” Y20 spherical harmonic; a Y20 with its axis of symmetry rotated to the equatorial plane. This – Editor: R.D. van der Hilst degree 2 signal, which continues with decreasing amplitude for more than 1000 km above the core mantle boundary (CMB), is characterized by two antipodal regions of low velocities, separated by a circum-polar Keywords: torus of higher than average velocities. If the slow regions are associated with net excess mass, then any axis mantle dynamics of rotation located in the plane of the circum-polar torus will be close to the maximum moment of inertia seismic tomography axis; this includes, of course, the current axis of rotation.