DOCSLIB.ORG

32Nd International Gemmological Conference IGC

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
32Nd International Gemmological Conference IGC 32nd International Gemmological Conference IGC July 2011 Interlaken, Switzerland 32nd IGC 2011 - Interlaken, Switzerland Introduction 32nd International Gemmological Conference IGC July 2011 Interlaken, Switzerland Dear Participant of the 32nd IGC Conference in Interlaken, Switzerland Two years after the last IGC Conference - organised by John Saul and his family in Arusha, Tanzania - it is our great pleasure to now host this event in Switzerland, 39 years after the last IGC Conference was held in Switzerland in 1972. The IGC has always been a platform to present and discuss the latest research in gemmology. But apart from this, it has also been a great opportunity to meet old and new friends and to share not only science, but also friendship during the meeting. In this spirit, I wish you in the name of the whole organising team an exciting and inspiring IGC Conference with lots of gemmological inputs for your own gemmological research and work. June 2011 Michael S. Krzemnicki, SSEF 2 32nd IGC 2011 - Interlaken, Switzerland Introduction About the organising Committee for the 32nd IGC Conference: Organisers Michael S. Krzemnicki, Swiss Gemmological Institute SSEF Laurent Cartier, Swiss Gemmological Institute SSEF George Bosshart Anne Bosshart Walter Balmer Henry A. Hänni, Swiss Gemmological Institute SSEF & GemExpert Michael Hügi, Swiss Gemmological Society SGS Thomas Frieden, Swiss Gemmological Society SGS, Frieden AG Local planning & Social programme: Walter Balmer Abstract Review Board: George Bosshart, Henry A. Hänni, Swiss Gemmological Institute SSEF & GemExpert, Layout & Editing & Website: Laurent Cartier, Swiss Gemmological Institute Organising an IGC Conference is only possible with a strong and committed team. I would like to thank my collea- gues for their support, which has made this conference possible. Special thanks go to: - George Bosshart for his trememdous work finalizing the abstract versions for the Conference Proceedings and Henry A. Hänni for reviewing the submitted abstracts. - Anne Bosshart for setting up a spectacular Accompanying programme in the heart of Switzerland. - Walter Balmer, who with his local „network“ in Interlaken (see also sponsors!) has been a great support for me, actually from the first moment when the decision was taken during the last IGC in Tanzania 2009 to host this Conference in Switzerland. Finally, I also would like to thank Laurent Cartier very much for his assistance in organising the Conference and the excursions, communicating with the participants, and layouting and editing the website and these Conference proceedings. June 2011 Michael. S. Krzemnicki 3 32nd IGC 2011 - Interlaken, Switzerland Introduction About the IGC Executive Board In 2009, four new members (Jayshree Panjikar, George Bosshart, Hanco Zwaan, and Michael S. Krzemnicki) joined the IGC Executive Board replacing long-standing Board members Dr. Jan Kanis, Mr. Alan Jobbins, Prof. Ichiro Suna- gawa, and Prof. Hermann Bank, who were awarded the honorary membership of the IGC in acknowledging the contributions they made to IGC in the past. Photo of the new IGC Executive Board, taken in October 2009 in Arusha: ! (From left to right) Hanco Zwaan, Jayshree Panjikar, George Bosshart, Emmanuel Fritsch, Tay Thye Sun, Gamini Zoysa, Michael S. Krzemnicki, John Saul, together with Mark Saul (standing). Not on the photo: John Koivula and Henry A. Hänni. Pre-conference excursion: 11-13 July 2011. Bern, Ticino and Swiss Alps. Conference: 13-17 July 2011. Interlaken, Switzerland. Post-conference excursion: 18-20 July 2011. Bernese Alps, Binn valley, Zermatt. Guest programme: 13-16 July 2011. Frutigen, Bern, Ballenberg, Lauterbrunnen, Schilthorn. 4 32nd IGC 2011 - Interlaken, Switzerland Introduction About the venue Interlaken Interlaken is a small town in the heart of Switzerland, beautifully located between the lakes of Brienz and Thun, and surrounded by the Swiss Alps, among them the famous Eiger, Mönch and Jungfrau with the train station „Top of Europe“ in the midst of glaciers. We have chosen Interlaken not only because of the conference infrastructure it offers, but mainly, because of the spectacular setting with plenty of possibilities to enjoy the Swiss nature and culture. The organising committee has planned a number of social activities, which include a visit to the Harder Kulm and the Gala Dinner at the Hotel Giessbach close to the famous Giessbach falls, not to mention a traditional Swiss folclore night with the hope to make you this Conference a lasting souvenir. Spectacular view on Interlaken and the Eiger, Mönch and Jungfrau summits. ! ! The Conference Venue The Conference will be held at the Interlaken Congress centre, perfectly equipped to host the 32nd IGC Confe- rence. We have at our disposition the Ballsaal (dancing room), where all presentations will be given. At the back of the Ballsaal, we the posters will be presented, together with a few product presentations of our sponsors. In the adjacent Rondell, the Interlaken Congress centre Catering will offer small snacks and coffee during coffee breaks and lunch during lunch breaks. ! 5 32nd IGC 2011 - Interlaken, Switzerland Introduction About the Sponsors The organisers would like to thank the following sponsors, which have kindly contributed with their sponsorship to organise the IGC Conference in Interlaken. Bödeli www.kabel-tv-boedeli.ch/ GemExpert www.gemexpert.ch Swiss Gemmological Institute SSEF www.ssef.ch Polytec GmbH www.polytec.de Bruker Switzerland www.bruker.ch System Eickhorst www.eickhorst 6 32nd IGC 2011 - Interlaken, Switzerland Conference Programme IGC 2011 Programme Interlaken, Switzerland 13-17 July 2011 Wednesday 13 July 18.00-20.30 IGC Welcome reception in Interlaken at the Grand Hotel Victoria Jungfrau 20.30-22.00 Executive Committee (EXECO) reunion Thursday 14 July Coloured Stones 9.00-9.20 Opening ceremony and Announcements 9.20-10.05 Invited lecture by Prof. T. Armbruster, University of Berne, Switzerland : Gemmology at the Interface between Mineralogy and Crystallography Tourmaline, Garnet, Spodumene, Spinel, Turquoise (Chairman John Koivula) 10.05-10.25 Karl Schmetzer et al : Trapiche tourmaline from Zambia –chemical and structural zoning 10.25-10.45 Federico Pezzotta et al: Gem tourmaline from Elba Island, Italy 10.45-11.05 Coffee break 11.05-11.25 Ulrich Henn et al: Mn-bearing grossular garnet 11.25-11.45 George Bosshart et al: Colorimetric investigation of unstable and stable spodumene colours 11.45-12.05 Furuya Masaki Colouring agents and their spectra in blue spinel 12.05-12.25 Jean Marie Dereppe et al : EPR of turquoise and some of its imitations 12.25-14.00 Lunch 7 32nd IGC 2011 - Interlaken, Switzerland Conference Programme Quartz, Opals (Chairman Lin Sutherland) 14.00-14.20 Jurgen Schnellrath et al.: Quartz cat’s eyes with unusual fibre distribution patterns 14.20-14.40 Claudio Milisenda et al : Irradiated blue common opal from Brazil 14.40-15.00 Benjamin Rondeau et al : Play-of-colour opal from Wollo, Ethiopia: a new pedogenetic model for gem opal formation 15.00-16.00 Poster session (see below) 15.40-16.00 Coffee break Beryls 16.00-16.20 Henry Hänni : Beryl – 30 years later 16.20-16.40 Liu Shang-I et al: Study of an extraordinary Cs- and Li-rich beryl from Madagascar 16.40-17.00 Hanco Zwaan et al. : Preliminary report on emeralds from the Fazenda Bonfim region, Rio Grande do Norte, Brazil 17.00 Conference closes 19.00 Meeting point Kursaal entrance for walk to Harder Kulm train station 19.30-22.00 Dinner at Harder Kulm Restaurant Friday 15 July Pearls / Diamonds 8.00-8.45 EXECO reunion Pearls (Chairman Hanco Zwaan) 9.00-9.20 Elisabeth Strack : An overview of production techniques for Chinese freshwater cultured pearls 9.20- 9.40 Michael Krzemnicki et al.: External and internal structures of Tokki pearls: additional cultured pearls formed during pearl cultivation 8 32nd IGC 2011 - Interlaken, Switzerland Conference Programme 9.40-10.00 Nick Sturman et al. Cultured Queen Conch pearls – A comparison to natural Queen Conch pearls 10.00-10.20 Federico Bärlocher : The natural Melo pearls from the Andaman Sea, Myanmar 10.20-10.40 Coffee break Diamonds (Chairman Karl Schmetzer) 10.40-11.00 Laurent Cartier Diamond production in Sierra Leone since 1930 11.00- 11.20 N. N. Zudina, et al.: Orange diamonds from the Siberian placers: the features of structural defects 11.20-11.40 Thomas Hainschwang et al.: Photoluminescence spectroscopy and imaging of type Ib diamonds 11.40-12.00 Emmanuel Fritsch et al.: ”Birefringence” in diamond: a useful tool to separate natural from synthetic diamond 12.00-12.05 Announcements 12.05-13.30 Lunch 13.30-14.20 Poster session (see below) Diamonds (Chairman Tay Thye Sun) 14.20-14.40 Yuri Shelementiev et al.: Distinction between well and poorly cut diamonds on the basis of dark zone analysis 14.40-15.00 Joe Yuan et al.: Using synchrotron radiation to analyse diamond crystal structure 15.00-15.20 Israel Eliezri: From Rough to Report – Use of Technology 15.20 Conference day closes 17.00 Meeting point Kursaal entrance for walk to boat pier Interlaken East 17.30 Boat leaves for Giessbach 19.00 Conference photograph will be taken with all participants at Giessbach 19.30-22.00 Gala Dinner at Giessbach Hotel 9 32nd IGC 2011 - Interlaken, Switzerland Conference Programme Saturday 16 July Coloured Stones Corundum, Heat treatment (Chairman Ulrich Henn) 9.00-9.20 Walter Balmer et al.: Re-assessment of the characterisation of UV-Vis spectra for rubies from marble-hosted deposits 9.20- 9.40 Jayshree Panjikar et
Load more

Recommended publications
  • Pallasites: Olivine-Metal Textures, Phosphoran Olivine, and Origin
    Pallasites: olivine-metal textures, phosphoranolivine, and origin Ed Scott University of Hawai’i, Honolulu, HI 96822. [email protected] Four questions: 3. Origin of the four FeO-rich MG pallasites 1. Why do some pallasites have rounded olivines? 2. Why is phosphoran olivine only found in five main-group pallasites? 3. Why do four main group pallasites with rounded olivines contain abnormally Fe-rich olivine? 4. Where did main group and Eagle Station group pallasites form? a 1. Origin of rounded olivine Did cm-sized rounded olivines form before angular olivines [9], or were olivines rounded after Fig. 5. Zaisho, Springwater, Rawlinna, and Phillips Co. fragmentation of olivine [2.3,7]? Constraints: contain anomalously Fe-rich olivine, Ni-rich metal, and • Uniform size distribution of rounded olivines in farringtonite Mg3(PO4)2 [20] suggesting Fe was oxidized. Fig.1c is unlike that of angular olivine pallasites Fig. 3. Ir vs. Ni showing metal in main group pallasites and IIIAB irons. Arrows show Data from [2]. which may contain dunite fragments several cm solid and liquid Fe-Ni paths during fractional crystallization. MG pallasites were b in width (Fig. 1a.). mostly formed by mixing of residual metallic liquid from a IIIAB-like core after 75- Springwater contains 4 • Angular olivine pallasites may contain pieces of 80% crystallization [1,2]. Pavlodar (Pa) has rounded olivines and plots near the vol.% farringtonite (center) rounded olivine texture (Fig. 1b). initial melt composition showing that rounding preceded metal crystallization. enclosing olivine. Slice ~12 • Pavlodar metal matches that expected for initial Marjalahti (Ma), Huckitta (Hu) and Seymchan (Se) have angular olivines and cm wide.
    [Show full text]
  • Elemental Abundances in the Metal of Los Vientos 263 - an Anomalous Pallasite Formed in a Reduced Environment
    50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1442.pdf ELEMENTAL ABUNDANCES IN THE METAL OF LOS VIENTOS 263 - AN ANOMALOUS PALLASITE FORMED IN A REDUCED ENVIRONMENT. S. Sharma1, M. Humayun1, R. Hewins2,3, B. Zanda2,4, J. Gattac- ceca5, C. Sonzogni5 and S. Sillitoe-Kukas1. 1Dept. Earth, Ocean & Atmospheric Science, and National High Magnet- ic Field Laboratory, Florida State University, Tallahassee, FL 32310, USA ([email protected]); 2IMPMC, UPMC, MNHN – UMR CNRS 7590, 75005 Paris, France; 3Dept. Earth & Planetary Sciences, Rutgers University, Pisca- taway, NJ 08854, USA; 4IMCCE, Observatoire de Paris - CNRS UMR 8028, 75014 Paris, France; 5Aix Marseille Univ., CNRS, IRD, Coll France, INRA, CEREGE, Aix-en-Provence, France. Introduction: Metal-rich meteorites bear important metal in LoV 263. It does not resemble any ungrouped information on the diversity of planetesimals in the irons in Ni-Ga-Ge relations (not shown). Early Solar System. Pallasites, olivine-metal bearing Table 1: Composition of the metal in LoV 263. meteorites, characterized by their mineralogy, chemis- try and oxygen isotopic composition, include the Main Conc. (ppm) Conc. (ppm) Group pallasites (PMG), the Eagle Station pallasites V 0.2 Ru 12.4 (PES), and many anomalous members [1, 2, 3]. A Cr 4 Rh 1.70 growing number of anomalous pyroxene-bearing pal- Fe 938000 Pd 1.55 lasites have been found that are distinct from the PMG Co 4020 Sn 0.47 and PES - Vermillion, Yamato 8451, Choteau, NWA Ni 56500 Sb 0.047 10019, Zinder and NWA 1911 [4,5]. Milton is another Cu 131 W 1.93 unique pallasite, which is similar to ES group in its Fa content with a distinct oxygen isotopic signature [6].
    [Show full text]
  • Unbroken Meteorite Rough Draft
    Space Visitors in Kentucky: Meteorites and Asteroid “Ida.” Most meteorites originate from asteroids. Meteorite Impact Sites in Kentucky Meteorite from Clark County, Ky. Mercury Earth Saturn Venus Mars Neptune Jupiter William D. Ehmann Asteroid Belt with contributions by Warren H. Anderson Uranus Pluto www.uky.edu/KGS Special thanks to Collie Rulo for cover design. Earth image was compiled from satellite images from NOAA and NASA. Kentucky Geological Survey James C. Cobb, State Geologist and Director University of Kentucky, Lexington Space Visitors in Kentucky: Meteorites and Meteorite Impact Sites in Kentucky William D. Ehmann Special Publication 1 Series XII, 2000 i UNIVERSITY OF KENTUCKY Collie Rulo, Graphic Design Technician Charles T. Wethington Jr., President Luanne Davis, Staff Support Associate II Fitzgerald Bramwell, Vice President for Theola L. Evans, Staff Support Associate I Research and Graduate Studies William A. Briscoe III, Publication Sales Jack Supplee, Director, Administrative Supervisor Affairs, Research and Graduate Studies Roger S. Banks, Account Clerk I KENTUCKY GEOLOGICAL SURVEY Energy and Minerals Section: James A. Drahovzal, Head ADVISORY BOARD Garland R. Dever Jr., Geologist V Henry M. Morgan, Chair, Utica Cortland F. Eble, Geologist V Ron D. Gilkerson, Vice Chair, Lexington Stephen F. Greb, Geologist V William W. Bowdy, Fort Thomas David A. Williams, Geologist V, Manager, Steven Cawood, Frankfort Henderson office Hugh B. Gabbard, Winchester David C. Harris, Geologist IV Kenneth Gibson, Madisonville Brandon C. Nuttall, Geologist IV Mark E. Gormley, Versailles William M. Andrews Jr., Geologist II Rosanne Kruzich, Louisville John B. Hickman, Geologist II William A. Mossbarger, Lexington Ernest E. Thacker, Geologist I Jacqueline Swigart, Louisville Anna E.
    [Show full text]
  • Machine Learning for Semi-Automated Meteorite Recovery
    Machine Learning for Semi-Automated Meteorite Recovery Seamus Anderson1*, Martin Towner1, Phil Bland1, Christopher Haikings2,3, William Volante4, Eleanor Sansom1, Hadrien Devillepoix1, Patrick Shober1, Benjamin Hartig1, Martin Cupak1, Trent Jansen- Sturgeon1, Robert Howie1, Gretchen Benedix1, Geoff Deacon5 1Space Science and Technology Center, Curtin University, GPO Box U1987, Perth, WA 6845, Australia 2Spectre UAV Concepts, 191 St Georges Terrace, Perth, WA 6000, Australia 3Amotus Pty Ltd, Level 25/71 Eagle St, Brisbane City, QLD 4000, Australia 4Department of Psychology, Clemson University, 418 Brackett Hall, Clemson, SC, 29634 5Western Australian Museum, 49 Kew St, Welshpool, WA 6106, Australia *Corresponding author: E-mail: [email protected]. Abstract We present a novel methodology for recovering meteorite falls observed and constrained by fireball networks, using drones and machine learning algorithms. This approach uses images of the local terrain for a given fall site to train an artificial neural network, designed to detect meteorite candidates. We have field tested our methodology to show a meteorite detection rate between 75-97%, while also providing an efficient mechanism to eliminate false-positives. Our tests at a number of locations within Western Australia also showcase the ability for this training scheme to generalize a model to learn localized terrain features. Our model-training approach was also able to correctly identify 3 meteorites in their native fall sites, that were found using traditional searching techniques. Our methodology will be used to recover meteorite falls in a wide range of locations within globe- spanning fireball networks. Introduction Fireballs and meteors have been observed since antiquity by Chinese, Korean, Babylonian and Roman astronomers (Bjorkman 1973), while meteorites and their unique metallurgical properties have also been known and used by various cultures around the world from Inuit tools (Rickard 1941) to an Egyptian ceremonial dagger (Comelli et al.
    [Show full text]
  • Geochemical Constraints on the Origin of the Moon and Preservation of Ancient Terrestrial Heterogeneities
    S. J. Lock et al., Space Science Reviews, 216, 109, doi: 10.1007/s11214-020-00729-z, 2020 Geochemical constraints on the origin of the Moon and preservation of ancient terrestrial heterogeneities Simon J. Locka,∗, Katherine R. Berminghamb,c, Rita Paraid, Maud Boyete aDivision of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA. bDepartment of Earth and Planetary Sciences, Rutgers University, Piscataway, NJ 08854, USA cDepartment of Geology, University of Maryland,College Park, MD 20742, USA. dDepartment of Earth and Planetary Sciences, Washington University in St. Louis, Saint Louis, MO 63130, USA. eUniversit´eClermont Auvergne, CNRS, IRD, OPGC, Laboratoire Magmas et Volcans, F-63000 Clermont-Ferrand, France. Abstract The Moon forming giant impact marks the end of the main stage of Earth's accretion and sets the stage for the subsequent evolution of our planet. The giant impact theory has been the accepted model of lunar origin for 40 years, but the parameters of the impact and the mechanisms that led to the formation of the Moon are still hotly debated. Here we review the principal geochemical observations that constrain the timing and parameters of the impact, the mechanisms of lunar formation, and the contemporaneous evolution of Earth. We discuss how chemical and isotopic studies on lunar, terrestrial and meteorite samples relate to physical models and how they can be used to differentiate between lunar origin models. In particular, we argue that the efficiency of mixing during the collision is a key test of giant impact models. A high degree of intra-impact mixing is required to explain the isotopic similarity between the Earth and Moon but, at the same time, the impact did not homogenize the whole terrestrial mantle, as isotopic signatures of pre-impact heterogeneity are preserved.
    [Show full text]
  • NI 43-101 Preliminary Economic Assessment Report
    N.I. 43-101 TECHNICAL REPORT & PRELIMINARY ECONOMIC ASSESSMENT FOR THE TURNAGAIN PROJECT – Amended British Columbia, Canada Report date: November 18, 2020 Amended report date: February 3, 2021 Effective date: October 28, 2020 Prepared for: Suite 203 – 700 West Pender St., Vancouver, BC, V6C 1G8 www.gigametals.com Prepared by: 1066 W. Hastings St., Vancouver, BC, V6E 3X2 Project Number: H-361523 Qualified Persons Ian Thompson, P.Eng., Persio Rosario, P.Eng., Evan Jones, P.Eng., & Gerald Schwab, P.Eng. – Hatch Ltd. • Garth Kirkham, P.Geo – Kirkham Geosystems • Daniel Friedman, P.Eng. – Knight Piésold • Ron Monk, P.Eng. – Kerr Wood Leidal • Chris Martin, C.Eng. MIMMM – Blue Coast Metallurgy • Andrew Mitchell, PhD, C.Eng – Wood Mackenzie Kirkham Geosystems Ltd. February 3, 2021 REPORT AMENDMENTS The attached report entitled “N.I. 43-101 Technical Report & Preliminary Economic Assessment For The Turnagain Project” (the “Technical Report”) prepared for Giga Metals Corporation and dated November 18, 2020 has been updated and refiled to provide the following additional detail and clarifying language: 1. In Section 1.12, the following wording was included “The preliminary economic assessment is preliminary in nature. It includes inferred mineral resources that are too speculative geologically to have economic considerations applied to them that would enable them to be categorised as mineral reserves, and there is no certainty that the preliminary economic assessment will be realized.” 2. The fourth paragraph of Section 1.13, the final paragraph of Section 25.1, and the first paragraph of Section 26.1 were edited to the following “This PEA indicates the Turnagain property generates an internal rate of return below the applied discount rate on the estimated N.I.
    [Show full text]
  • Petrogenesis of Main Group Pallasite Meteorites Based on Relationships
    Vrije Universiteit Brussel Petrogenesis of main group pallasite meteorites based on relationships among texture, mineralogy, and geochemistry Mckibbin, Seann; Pittarello, Lidia; Makarona, Christina; Hamman, Christopher; Hecht, Lutz; Chernonozhkin, Stepan; Goderis, Steven; Claeys, Philippe Published in: Meteoritics & Planetary Science DOI: 10.1111/maps.13392 Publication date: 2019 Link to publication Citation for published version (APA): Mckibbin, S., Pittarello, L., Makarona, C., Hamman, C., Hecht, L., Chernonozhkin, S., ... Claeys, P. (2019). Petrogenesis of main group pallasite meteorites based on relationships among texture, mineralogy, and geochemistry. Meteoritics & Planetary Science, 54(11), 2814-2844. https://doi.org/10.1111/maps.13392 General rights Copyright and moral rights for the publications made accessible in the public portal are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. • Users may download and print one copy of any publication from the public portal for the purpose of private study or research. • You may not further distribute the material or use it for any profit-making activity or commercial gain • You may freely distribute the URL identifying the publication in the public portal Take down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Download date: 03. Oct. 2021 Meteoritics & Planetary Science 1–31 (2019) doi: 10.1111/maps.13392 Petrogenesis of main group pallasite meteorites based on relationships among texture, mineralogy, and geochemistry 1,5,6* 1,7 1 Seann J.
    [Show full text]
  • Independent Ni 43-101 Technical Report on the Bannockburn Nickel Sulphide Project
    INDEPENDENT NI 43-101 TECHNICAL REPORT ON THE BANNOCKBURN NICKEL SULPHIDE PROJECT Matachewan Area Ontario, Canada PREPARED FOR: Grid Metals Corp. 3335 Yonge Street, Suite 304 Toronto, Ontario M4N 2M1, Canada PREPARED BY: Caracle Creek International Consulting Inc. 1545 Maley Drive, Suite 2018 Sudbury, Ontario P3A 4R7, Canada Effective Date: December 31, 2020 Issue Date: January 19, 2021 Qualified Persons: Dr. Scott Jobin-Bevans (PhD, P.Geo., PMP) Principal Geoscientist Mr. Paul Davis (M.Sc., P.Geo.) Geoscientist Project Number: 605.20.00 Grid Metals Corp: Bannockburn Nickel, Ontario, Canada NI 43-101 Technical Report January 19, 2021 DATE AND SIGNATURE The Report, “Independent NI 43-101 Technical Report on the Bannockburn Nickel Sulphide Project, Matachewan Area, Ontario, Canada”, dated the 19th January 2021, with an Effective Date of the 31st December 2020, and prepared for Grid Metals Corp., was authored by the following: “signed and sealed original on file” _______________________________________ Scott Jobin-Bevans (PhD, P.Geo. #0183, PMP) Principal Geoscientist Caracle Creek International Consulting Inc. (Canada) “signed and sealed original on file” _______________________________________ Paul Davis (M.Sc., P.Geo. #1109) Geoscientist Paul Davis Consulting Dated: January 19, 2021 Caracle Creek International Consulting Page i of vi Grid Metals Corp: Bannockburn Nickel, Ontario, Canada NI 43-101 Technical Report January 19, 2021 TABLE OF CONTENTS Table of Contents .......................................................................................................................................
    [Show full text]
  • The Compositional Structure of the Asteroid Belt
    The Compositional Structure of the Asteroid Belt F. E. DeMeo Massachusetts Institute of Technology C. M. O’D. Alexander Carnegie Institution of Washington K. J. Walsh and C. R. Chapman Southwest Research Institute R. P. Binzel Massachusetts Institute of Technology Abstract: The past decade has brought major improvements in large-scale asteroid discovery and characterization with over half a million known asteroids and over 100,000 with some measurement of physical characterization. This explosion of data has allowed us to create a new global picture of the Main Asteroid Belt. Put in context with meteorite measurements and dynamical models, a new and more complete picture of Solar System evolution has emerged. The question has changed from “What was the original compositional gradient of the Asteroid Belt?” to “What was the original compositional gradient of small bodies across the entire Solar System?” No longer is the leading theory that two belts of planetesimals are primordial, but instead those belts were formed and sculpted through evolutionary processes after Solar System formation. This article reviews the advancements on the fronts of asteroid compositional characterization, meteorite measurements, and dynamical theories in the context of the heliocentric distribution of asteroid compositions seen in the Main Belt today. This chapter also reviews the major outstanding questions relating to asteroid compositions and distributions and summarizes the progress and current state of understanding of these questions to form the big picture of the formation and evolution of asteroids in the Main Belt. Finally, we briefly review the relevance of asteroids and their compositions in their greater context within our Solar System and beyond.
    [Show full text]
  • Rare, Metal Micrometeorites from the Indian Ocean M
    1 Author Version : Meteoritics & Planetary Science, vol.54(2); 2019; 290-299 Rare, metal micrometeorites from the Indian Ocean M. Shyam Prasad*, N.G. Rudraswami, Agnelo Alexandre de Araujo, and V.D. Khedekar Geological Oceanography Division CSIR- National Institute of Oceanography Dona Paula, Goa – 403004, INDIA *[email protected] ABSTRACT Metal in various forms is common in almost all meteorites but considerably rare among micrometeorites. We report here the discovery of two metal micrometeorites : 1. An awaruite grain similar to those found in the metal nodules of CV chondrites. 2. Metal micrometeorite of kamacite composition enclosing inclusions of chromite and merrillite. This micrometeorite appears to be a fragment of H5/L5 chondrite. These metal micrometeorites add to the inventory of solar system materials that are accreted by the earth in the microscopic form. They also strengthen the argument that a large proportion of material accreted by the earth that survives atmospheric entry is from asteroidal sources. 2 INTRODUCTION Fe-Ni metal is a common constituent of most meteorites and is a sensitive indicator of the metamorphism, thermal history undergone by the respective meteorites, therefore it is a diagnostic tool to understand redox conditions in the nebula and also to distinguish between groups/sub-groups of meteorites (Wood 1967; Afiatalab and Wasson, 1980; Rubin, 1990, Kimura et al. 2008; Smith et al. 1993). The metal is present in the form of kamacite (most common), plessite, taenite, Fe-Ni-S, and also as beads of Fe-Ni (Brearley and Jones, 1998). There are rare metallic minerals such as the awaruite, buchwaldite, schreibersite etc., reported exclusively from different meteorites (Rubin, 1997), such minerals are never reported from the micrometeorites although they constitute a predominant fraction of the extraterrestrial flux.
    [Show full text]
  • Some Australian Contributions to Meteoritics from the 19Th to the 21St Centuries
    WA Science—Journal of the Royal Society of Western Australia, 97: 237–252, 2014 Some Australian contributions to meteoritics from the 19th to the 21st Centuries A W R BEVAN Department of Earth and Planetary Sciences, Western Australian Museum, Locked Bag 49, Welshpool DC, WA 6986, Australia. [email protected] Meteorites are fragments of natural debris that survive their fall to Earth from space, and meteoritics is the science of their study. Meteorites are fundamental to our understanding of the origin and early evolution of the Solar System. Many have remained virtually unaltered for 4.56 Ga and represent some of the original materials from which the planets were constructed. From the 19th Century onwards contributions to the understanding of planetary materials have been made by Australian scientists in the fields of meteorite recovery, mineralogy, petrology and metallurgy of meteorites, meteorite classification, isotopic studies, geochronology, impact cratering and Solar System formation. This paper documents some of the significant achievements that have been made. KEYWORDS: chondrites, geochronology, irons, isotopes, meteorites, mineralogy, petrology, stony-irons. INTRODUCTION predominantly of silicates (olivine, pyroxene and feldspar) similar to those occurring in terrestrial basalts, Meteorites are a fundamental source of information on but may also contain appreciable amounts of metal; and the origin and early evolution of the Solar System, and stony-irons are mixtures of metal and silicates in roughly meteoritics is the science of their study. The majority of equal proportions. Stony meteorites are the most meteorites are fragments broken from asteroids in solar common, accounting for more than 95% of those orbits between Mars and Jupiter, although few specific observed to fall, whereas irons and stony-irons are rare, asteroids have been identified as possible sources.
    [Show full text]
  • Preliminary Paleomagnetic Analysis of the Eagle Station Pallasite
    45th Lunar and Planetary Science Conference (2014) 1945.pdf PRELIMINARY PALEOMAGNETIC ANALYSIS OF THE EAGLE STATION PALLASITE. J. A. Tar- duno1,2, R. D. Cottrell1, L. Ferrière3, and E. R. D. Scott4, 1Department of Earth & Environmental Sciences, Univer- sity of Rochester, Rochester, NY 14627 ([email protected]), 2Department of Physics & Astronomy, Uni- versity of Rochester, Rochester, NY 14627, 3Natural History Museum Vienna, Vienna A-1010, Austria, 4Hawaii Institute for Geophysics and Planetology, University of Hawaii, Manoa, HI 96822. Introduction: Remanent magnetizations recorded group include diopside, chromite, stanfieldite, whit- in minute FeNi inclusions in olivine from the Esquel, lockite, schreibersite, sphalerite, daubreelite and Imilac [1] and Springwater [2] meteorites record strong mackinawite [9]. Phosphates in the Eagle Station have paleointensities that require the presence of an inter- low concentrations of rare earth elements [10]. Olivine nally-generated dynamo in the main group pallasite in the Eagle Station pallasite is angular (versus parent body. The magnetizations are incompatible with rounded). a core-mantle boundary origin for these main group pallasites. Instead, injection of liquid FeNi metal from Methods: We report magnetic data from a sample the core of an impactor into the shallow mantle of the of the Eagle Station pallasite obtained from the Vienna Natural History Museum (Figure 1). We use an ap- main group pallasite parent body [1] can explain the proach for retrieving paleomagnetic data that uses sin- magnetic data and available cooling rate constraints gle silicate crystals [11]. Such crystals can contain [3]. Here, we examine the Eagle Station (Figure 1) minute magnetic inclusions (in the single to pseudo- pallasite to learn whether its magnetic signature can single domain range) that are magnetically stable on similarly constrain the nature of its parent body.
    [Show full text]