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Assembly, Configuration, and Break-Up History of Rodinia
Author's personal copy Available online at www.sciencedirect.com Precambrian Research 160 (2008) 179–210 Assembly, configuration, and break-up history of Rodinia: A synthesis Z.X. Li a,g,∗, S.V. Bogdanova b, A.S. Collins c, A. Davidson d, B. De Waele a, R.E. Ernst e,f, I.C.W. Fitzsimons g, R.A. Fuck h, D.P. Gladkochub i, J. Jacobs j, K.E. Karlstrom k, S. Lu l, L.M. Natapov m, V. Pease n, S.A. Pisarevsky a, K. Thrane o, V. Vernikovsky p a Tectonics Special Research Centre, School of Earth and Geographical Sciences, The University of Western Australia, Crawley, WA 6009, Australia b Department of Geology, Lund University, Solvegatan 12, 223 62 Lund, Sweden c Continental Evolution Research Group, School of Earth and Environmental Sciences, University of Adelaide, Adelaide, SA 5005, Australia d Geological Survey of Canada (retired), 601 Booth Street, Ottawa, Canada K1A 0E8 e Ernst Geosciences, 43 Margrave Avenue, Ottawa, Canada K1T 3Y2 f Department of Earth Sciences, Carleton U., Ottawa, Canada K1S 5B6 g Tectonics Special Research Centre, Department of Applied Geology, Curtin University of Technology, GPO Box U1987, Perth, WA 6845, Australia h Universidade de Bras´ılia, 70910-000 Bras´ılia, Brazil i Institute of the Earth’s Crust SB RAS, Lermontova Street, 128, 664033 Irkutsk, Russia j Department of Earth Science, University of Bergen, Allegaten 41, N-5007 Bergen, Norway k Department of Earth and Planetary Sciences, Northrop Hall University of New Mexico, Albuquerque, NM 87131, USA l Tianjin Institute of Geology and Mineral Resources, CGS, No. -
1 John A. Tarduno
JOHN A. TARDUNO January, 2016 Professor of Geophysics Tel: 585-275-5713 Department of Earth and Environmental Sciences Fax: 585-244-5689 University of Rochester, Rochester, NY 14627 Email: [email protected] USA http://www.ees.rochester.edu/people/faculty/tarduno_john Academic Career: 2005-present Professor of Physics and Astronomy, University of Rochester, Rochester, NY. 2000-present Professor of Geophysics, University of Rochester, Rochester, NY. 1998-2006 Chair, Department of Earth and Environmental Sciences 1996 Associate Professor of Geophysics, University of Rochester, Rochester, NY. 1993 Assistant Professor of Geophysics, University of Rochester, Rochester, NY. 1990 Assistant Research Geophysicist, Scripps Institution of Oceanography, La Jolla, Ca. 1989 National Science Foundation Postdoctoral Fellow, ETH, Zürich, Switzerland 1988 JOI/USSAC Ocean Drilling Fellow, Stanford University, Stanford, Ca. 1987 Ph.D. (Geophysics), Stanford University, Stanford, Ca. 1987 M.S. (Geophysics) Stanford University, Stanford Ca. 1983 B.S. (Geophysics) Lehigh University, Bethlehem Pa. Honors and Awards: Phi Beta Kappa (1983) Fellow, Geological Society of America (1998) JOI/USSAC Distinguished Lecturer (2000-2001) Goergen Award for Distinguished Achievement and Artistry in Undergraduate Teaching (2001) Fellow, American Association for the Advancement of Science (2003) American Geophysical Union/Geomagnetism and Paleomagnetism Section Bullard Lecturer (2004) Fellow, John Simon Guggenheim Foundation (2006-2007) Edward Peck Curtis Award for -
The Water on Mars Vanished. This Might Be Where It Went
The water on Mars vanished. This might be where it went. timesofindia.indiatimes.com/home/science/the-water-on-mars-vanished-this-might-be-where- it-went-/articleshow/81599751.cms NYT News Service | Mar 20, 2021, 10:32 IST Mars was once wet, with an ocean’s worth of water on its surface. Today, most of Mars is as dry as a desert except for ice deposits in its polar regions. Where did the rest of the water go? Some of it disappeared into space. Water molecules, pummeled by particles of solar wind, broke apart into hydrogen and oxygen atoms, and those, especially the lighter hydrogen atoms, sped out of the atmosphere, lost to outer space. A tall outcropping of rock, with layered deposits of sediments in the distance, marking a remnant of an ancient, long-vanished river delta in Jezero Crater, are pictured in this undated image taken by NASA's Mars rover Perseverance. (Reuters) But most of the water, a new study concludes, went down, sucked into the red planet’s rocks. And there it remains, trapped within minerals and salts. Indeed, as much as 99% of the water that once flowed on Mars could still be there, the researchers estimated in a paper published this week in the journal Science. Data from the past two decades of robotic missions to Mars, including NASA ’s Curiosity rover and the Mars Reconnaissance Orbiter, showed a wide distribution of what geologists call hydrated minerals. “It became very, very clear that it was common and not rare to find evidence of water alteration,” said Bethany Ehlmann, a professor of planetary science at the California Institute of Technology and one of the authors of the paper. -
Geophysical Field Mapping
Presented at Short Course IX on Exploration for Geothermal Resources, organized by UNU-GTP, GDC and KenGen, at Lake Bogoria and Lake Naivasha, Kenya, Nov. 2-23, 2014. Kenya Electricity Generating Co., Ltd. GEOPHYSICAL FIELD MAPPING Anastasia W. Wanjohi, Kenya Electricity Generating Company Ltd. Olkaria Geothermal Project P.O. Box 785-20117, Naivasha KENYA [email protected] or [email protected] ABSTRACT Geophysics is the study of the earth by the quantitative observation of its physical properties. In geothermal geophysics, we measure the various parameters connected to geological structure and properties of geothermal systems. Geophysical field mapping is the process of selecting an area of interest and identifying all the geophysical aspects of the area with the purpose of preparing a detailed geophysical report. The objective of geophysical field work is to understand all physical parameters of a geothermal field and be able to relate them with geological phenomenons and come up with plausible inferences about the system. Four phases are involved and include planning/desktop studies, reconnaissance, actual data aquisition and report writing. Equipments must be prepared and calibrated well. Geophysical results should be processed, analysed and presented in the appropriate form. A detailed geophysical report should be compiled. This paper presents the reader with an overview of how to carry out geophysical mapping in a geothermal field. 1. INTRODUCTION Geophysics is the study of the earth by the quantitative observation of its physical properties. In geothermal geophysics, we measure the various parameters connected to geological structure and properties of geothermal systems. In lay man’s language, geophysics is all about x-raying the earth and involves sending signals into the earth and monitoring the outcome or monitoring natural signals from the earth. -
Mantle Flow Through the Northern Cordilleran Slab Window Revealed by Volcanic Geochemistry
Downloaded from geology.gsapubs.org on February 23, 2011 Mantle fl ow through the Northern Cordilleran slab window revealed by volcanic geochemistry Derek J. Thorkelson*, Julianne K. Madsen, and Christa L. Sluggett Department of Earth Sciences, Simon Fraser University, Burnaby, British Columbia V5A 1S6, Canada ABSTRACT 180°W 135°W 90°W 45°W 0° The Northern Cordilleran slab window formed beneath west- ern Canada concurrently with the opening of the Californian slab N 60°N window beneath the southwestern United States, beginning in Late North Oligocene–Miocene time. A database of 3530 analyses from Miocene– American Holocene volcanoes along a 3500-km-long transect, from the north- Juan Vancouver Northern de ern Cascade Arc to the Aleutian Arc, was used to investigate mantle Cordilleran Fuca conditions in the Northern Cordilleran slab window. Using geochemi- Caribbean 30°N Californian Mexico Eurasian cal ratios sensitive to tectonic affi nity, such as Nb/Zr, we show that City and typical volcanic arc compositions in the Cascade and Aleutian sys- Central African American Cocos tems (derived from subduction-hydrated mantle) are separated by an Pacific 0° extensive volcanic fi eld with intraplate compositions (derived from La Paz relatively anhydrous mantle). This chemically defi ned region of intra- South Nazca American plate volcanism is spatially coincident with a geophysical model of 30°S the Northern Cordilleran slab window. We suggest that opening of Santiago the slab window triggered upwelling of anhydrous mantle and dis- Patagonian placement of the hydrous mantle wedge, which had developed during extensive early Cenozoic arc and backarc volcanism in western Can- Scotia Antarctic Antarctic 60°S ada. -
Concepts and Approaches for Mars Exploration1
June 24, 2012 Concepts and Approaches for Mars Exploration1 ‐ Report of a Workshop at LPI, June 12‐14, 2012 – Stephen Mackwell2 (LPI) Michael Amato (NASA Goddard), Bobby Braun (Georgia Institute of Technology), Steve Clifford (LPI), John Connolly (NASA Johnson), Marcello Coradini (ESA), Bethany Ehlmann (Caltech), Vicky Hamilton (SwRI), John Karcz (NASA Ames), Chris McKay (NASA Ames), Michael Meyer (NASA HQ), Brian Mulac (NASA Marshall), Doug Stetson (SSECG), Dale Thomas (NASA Marshall), and Jorge Vago (ESA) Executive Summary Recent deep cuts in the budget for Mars exploration at NASA necessitate a reconsideration of the Mars robotic exploration program within NASA’s Science Mission Directorate (SMD), especially in light of overlapping requirements with future planning for human missions to the Mars environment. As part of that reconsideration, a workshop on “Concepts and Approaches for Mars Exploration” was held at the USRA Lunar and Planetary Institute in Houston, TX, on June 12‐14, 2012. Details of the meeting, including abstracts, video recordings of all sessions, and plenary presentations, can be found at http://www.lpi.usra.edu/meetings/marsconcepts2012/. Participation in the workshop included scientists, engineers, and graduate students from academia, NASA Centers, Federal Laboratories, industry, and international partner organizations. Attendance was limited to 185 participants in order to facilitate open discussion of the critical issues for Mars exploration in the coming decades. As 390 abstracts were submitted by individuals interested in participating in the workshop, the Workshop Planning Team carefully selected a subset of the abstracts for presentation based on their appropriateness to the workshop goals, and ensuring that a broad diverse suite of concepts and ideas was presented. -
Geological Evolution of the Red Sea: Historical Background, Review and Synthesis
See discussions, stats, and author profiles for this publication at: https://www.researchgate.net/publication/277310102 Geological Evolution of the Red Sea: Historical Background, Review and Synthesis Chapter · January 2015 DOI: 10.1007/978-3-662-45201-1_3 CITATIONS READS 6 911 1 author: William Bosworth Apache Egypt Companies 70 PUBLICATIONS 2,954 CITATIONS SEE PROFILE Some of the authors of this publication are also working on these related projects: Near and Middle East and Eastern Africa: Tectonics, geodynamics, satellite gravimetry, magnetic (airborne and satellite), paleomagnetic reconstructions, thermics, seismics, seismology, 3D gravity- magnetic field modeling, GPS, different transformations and filtering, advanced integrated examination. View project Neotectonics of the Red Sea rift system View project All content following this page was uploaded by William Bosworth on 28 May 2015. The user has requested enhancement of the downloaded file. All in-text references underlined in blue are added to the original document and are linked to publications on ResearchGate, letting you access and read them immediately. Geological Evolution of the Red Sea: Historical Background, Review, and Synthesis William Bosworth Abstract The Red Sea is part of an extensive rift system that includes from south to north the oceanic Sheba Ridge, the Gulf of Aden, the Afar region, the Red Sea, the Gulf of Aqaba, the Gulf of Suez, and the Cairo basalt province. Historical interest in this area has stemmed from many causes with diverse objectives, but it is best known as a potential model for how continental lithosphere first ruptures and then evolves to oceanic spreading, a key segment of the Wilson cycle and plate tectonics. -
Bethany L. Ehlmann California Institute of Technology 1200 E. California Blvd. MC 150-21 Pasadena, CA 91125 USA Ehlmann@Caltech
Bethany L. Ehlmann California Institute of Technology [email protected] 1200 E. California Blvd. Caltech office: +1 626.395.6720 MC 150-21 JPL office: +1 818.354.2027 Pasadena, CA 91125 USA Fax: +1 626.568.0935 EDUCATION Ph.D., 2010; Sc. M., 2008, Brown University, Geological Sciences (advisor, J. Mustard) M.Sc. by research, 2007, University of Oxford, Geography (Geomorphology; advisor, H. Viles) M.Sc. with distinction, 2005, Univ. of Oxford, Environ. Change & Management (advisor, J. Boardman) A.B. summa cum laude, 2004, Washington University in St. Louis (advisor, R. Arvidson) Majors: Earth & Planetary Sciences, Environmental Studies; Minor: Mathematics International Baccalaureate Diploma, Rickards High School, Tallahassee, Florida, 2000 Additional Training: Nordic/NASA Summer School: Water, Ice and the Origin of Life in the Universe, Iceland, 2009 Vatican Observatory Summer School in Astronomy &Astrophysics, Castel Gandolfo, Italy, 2005 Rainforest to Reef Program: Marine Geology, Coastal Sedimentology, James Cook Univ., Australia, 2004 School for International Training, Development and Conservation Program, Panamá, Sept-Dec 2002 PROFESSIONAL EXPERIENCE Professor of Planetary Science, Division of Geological & Planetary Sciences, California Institute of Technology, Assistant Professor 2011-2017, Professor 2017-present; Associate Director, Keck Institute for Space Studies 2018-present Research Scientist, Jet Propulsion Laboratory, California Institute of Technology, 2011-2020 Lunar Trailblazer, Principal Investigator, 2019-present MaMISS -
Sterngeryatctnphys18.Pdf
Tectonophysics 746 (2018) 173–198 Contents lists available at ScienceDirect Tectonophysics journal homepage: www.elsevier.com/locate/tecto Subduction initiation in nature and models: A review T ⁎ Robert J. Sterna, , Taras Geryab a Geosciences Dept., U Texas at Dallas, Richardson, TX 75080, USA b Institute of Geophysics, Dept. of Earth Sciences, ETH, Sonneggstrasse 5, 8092 Zurich, Switzerland ARTICLE INFO ABSTRACT Keywords: How new subduction zones form is an emerging field of scientific research with important implications for our Plate tectonics understanding of lithospheric strength, the driving force of plate tectonics, and Earth's tectonic history. We are Subduction making good progress towards understanding how new subduction zones form by combining field studies to Lithosphere identify candidates and reconstruct their timing and magmatic evolution and undertaking numerical modeling (informed by rheological constraints) to test hypotheses. Here, we review the state of the art by combining and comparing results coming from natural observations and numerical models of SI. Two modes of subduction initiation (SI) can be identified in both nature and models, spontaneous and induced. Induced SI occurs when pre-existing plate convergence causes a new subduction zone to form whereas spontaneous SI occurs without pre-existing plate motion when large lateral density contrasts occur across profound lithospheric weaknesses of various origin. We have good natural examples of 3 modes of subduction initiation, one type by induced nu- cleation of a subduction zone (polarity reversal) and two types of spontaneous nucleation of a subduction zone (transform collapse and plumehead margin collapse). In contrast, two proposed types of subduction initiation are not well supported by natural observations: (induced) transference and (spontaneous) passive margin collapse. -
Satellite Measured Ionospheric Magnetic Field Variations Over Natural Hazards Sites
remote sensing Article Satellite Measured Ionospheric Magnetic Field Variations over Natural Hazards Sites Christoph Schirninger 1,†, Hans U. Eichelberger 1,*,†, Werner Magnes 1 , Mohammed Y. Boudjada 1,†, Konrad Schwingenschuh 1,†, Andreas Pollinger 1, Bruno P. Besser 1, Pier F. Biagi 2 , Maria Solovieva 3, Jindong Wang 4, Bingjun Cheng 4, Bin Zhou 4, Xuhui Shen 5, Magda Delva 1 and Roland Lammegger 6 1 Space Research Institute, Austrian Academy of Sciences, Schmiedlstraße 6, 8042 Graz, Austria; [email protected] (C.S.); [email protected] (W.M.); [email protected] (M.Y.B.); [email protected] (K.S.); [email protected] (A.P.); [email protected] (B.P.B.); [email protected] (M.D.) 2 Department of Physics, University of Bari, 70126 Bari, Italy; [email protected] 3 Schmidt Institute of Physics of the Earth, Russian Academy of Sciences, 123995 Moscow, Russia; [email protected] 4 National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China; [email protected] (J.W.); [email protected] (B.C.); [email protected] (B.Z.) 5 National Institute of Natural Hazards, MEMC, Beijing 100085, China; [email protected] 6 Institute of Experimental Physics, Graz University of Technology, 8010 Graz, Austria; [email protected] * Correspondence: [email protected] † These authors contributed equally to this work. Citation: Schirninger, C.; Eichelberger, H.U.; Magnes, W.; Abstract: Processes and threats related to natural hazards play an important role in the evolution of Boudjada, M.Y.; Schwingenschuh, K.; the Earth and in human history. -
Role of Glaciers in Halting Syrtis Major Lava Flows to Preserve and Divert a Fluvial System
ROLE OF GLACIERS IN HALTING SYRTIS MAJOR LAVA FLOWS TO PRESERVE AND DIVERT A FLUVIAL SYSTEM A Thesis Submitted to the Graduate Faculty of the Louisiana State University and Agricultural and Mechanical College in partial fulfillment of the requirements for the degree of Master of Geology in The Department of Geology and Geophysics by Connor Michael Matherne B.S., Louisiana State University, 2017 December 2019 ACKNOWLEDGMENTS Special thanks to J.R. Skok and Jack Mustard for conceiving the initial ideas behind this project and to Suniti Karunatillake and J.R. Skok for their guidance. Additionally, thank you to my committee members Darrell Henry and Peter Doran for aid in understanding the complex volcanic and climate history for this location. This work has benefited from reviews and discussions with Tim Goudge, Steven Ruff, Jim Head, and Bethany Ehlmann. We thank Caleb Fassett for providing the CTX DEM processing of the outlet fan and Tim Goudge for providing the basin Depression CTX DEM. All data and observations used in this study are publically available from the NASA PDS. Derived products such as produced CTX DEMs can be attained through processing or contacting the primary author. Connor Matherne was supported by the Frank’s Chair funds, W.L. Calvert Memorial Scholarship, NASA-EPSCoR funded LASpace Graduate Student Research Assistantship grant, and Louisiana Board of Regents Research Award Program grant LEQSF-EPS(2017)-RAP-22 awarded to Karunatillake. J.R. Skok was supported with the MDAP award NNX14AR93G. Suniti Karunatillake’s work was supported by NASA- MDAP grant 80NSSC18K1375. ii TABLE OF CONTENTS Acknowledgments.............................................................................................................. -
Petrology on Mars†K
American Mineralogist, Volume 100, pages 2380–2395, 2015 INVITED CENTENNIAL ARTICLE REVIEW Petrology on Mars†k HARRY Y. MCSWEEN JR.1,* 1Department of Earth and Planetary Sciences and Planetary Geoscience Institute, University of Tennessee, Knoxville, Tennessee 37996-1410, U.S.A. ABSTRACT Petrologic investigations of martian rocks have been accomplished by mineralogical, geochemical, and textural analyses from Mars rov- ers (with geologic context provided by orbiters), and by laboratory analyses of martian meteorites. Igneous rocks are primarily lavas and volcaniclastic rocks of basaltic composition, and ultramafic cumulates; alkaline rocks are common in ancient terranes and tholeiitic rocks occur in younger terranes, suggesting global magmatic evolution. Relatively uncommon feldspathic rocks represent the ultimate fractionation prod- ucts, and granitic rocks are unknown. Sedimentary rocks are of both clastic (mudstone, sandstone, conglomerate, all containing significant igneous detritus) and chemical (evaporitic sulfate and less common carbonate) origin. High-silica sediments formed by hydrothermal activity. Sediments on Mars formed from different protoliths and were weathered under different environmental conditions from terrestrial sediments. Metamorphic rocks have only been inferred from orbital remote-sensing measurements. Metabasalt and serpentinite have mineral assemblages consistent with those predicted from low-pressure phase equilibria and likely formed in geothermal systems. Shock effects are com- mon in martian meteorites, and impact breccias are probably widespread in the planet’s crustal rocks. The martian rock cycle during early periods was similar in many respects to that of Earth. However, without plate tectonics Mars did not experience the thermal metamorphism and flux melting associated with subduction, nor deposition in subsided basins and rapid erosion resulting from tectonic uplift.