Uranium and Geology" (1908)
Total Page:16
File Type:pdf, Size:1020Kb

Load more
Recommended publications
-
John Joly (1857–1933)
Trinity College Memorial Discourse Monday 14th May 2007 JOHN JOLY (1857–1933) Patrick N. Wyse Jackson FTCD Department of Geology, Trinity College, Dublin 2, Ireland ([email protected]) Provost, Fellows, Scholars, Colleagues, Honoured Guests, and Friends It gives me great pleasure to be here today as we honour a Trinity scientist and life-long servant, and remember him close to the 150th anniversary of his birth in a small rural rectory in what is now County Offaly. I am also using the occasion to privately (and now that I mention it, publicly) remember another Trinity graduate, whose centenary his family will celebrate next year. On Trinity Monday, 67 years ago, my father Robert Wyse Jackson delivered the Memorial Discourse on Jonathan Swift. John Joly whom we honour today was a scientist with a vivid and clear imagination, and his research led him into many varied disciplines. He was a physicist, engineer, geophysicist, and educationalist, but also researched in botany, medicine and on photography. He was also closely associated with a number of Dublin organisations most notably the Royal Dublin Society of which he was President for a time, and with Alexandra College of which he was Warden for many years. This Discourse shall follow a broadly chronological sequence from his birth to death, and will examine various strands of his work and life either in depth to some degree, or else fleetingly. A bibliography of papers on Joly’s life and work is appended to the end of this Discourse. 1 John Joly in 1903 In adulthood Joly Joly was very distinctive. -
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 -
Publications
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Can perchlorates be transformed to hydrogen peroxide (H2O2) 10.1002/2017JE005329 products by cosmic rays on the Martian surface? Key Points: Parker B. Crandall1,2 , Sándor Góbi1,2, Jeffrey Gillis-Davis3, and Ralf I. Kaiser1,2 • Magnesium perchlorate samples were irradiated with deuterium ions and 1Department of Chemistry, University of Hawai’iatMānoa, Honolulu, Hawaii, USA, 2W.M. Keck Laboratory in Astrochemistry, electrons to model galactic cosmic ray ’ ā 3 ’ (GCR) exposure University of Hawai iatM noa, Honolulu, Hawaii, USA, Hawai i Institute of Geophysics and Planetology, University of • GCRs supplanted in the regolith can Hawai’iatMānoa, Honolulu, Hawaii, USA participate in the formation of hydrogen peroxide via the destruction À of perchlorates Abstract Due to their oxidizing properties, perchlorates (ClO4 ) are suggested by the planetary science • Volatile oxidizing agents formed likely community to play a vital role in the scarcity of organics on the Martian surface. However, alternative contribute to the lack of organic material beneath the Martian surface oxidation agents such as hydrogen peroxide (H2O2) have received surprisingly little attention. In this study, samples of magnesium perchlorate hexahydrate (Mg(ClO4)2 ·6H2O) were exposed to monoenergetic + electrons and D2 ions separately, sequentially, and simultaneously to probe the effects of galactic cosmic ray Correspondence to: exposure of perchlorates and the potential incorporation of hydrogen (deuterium) into these minerals. The R. I. Kaiser, experiments were carried out under ultrahigh-vacuum conditions at 50 K, after which the samples were [email protected] slowly heated to 300 K while the subliming products were monitored by a quadrupole mass spectrometer. -
MARS STUDENT IMAGING PROJECT FINAL REPORT ASU MARS EDUCATION PROGRAM Waubonsie Valley High School | Period 1 | 12‐13 School Year
MARS STUDENT IMAGING PROJECT FINAL REPORT ASU MARS EDUCATION PROGRAM Waubonsie Valley High School | Period 1 | 12‐13 School Year I. Introduction What is your science question? What effect do the polar ice caps have on craters in the rock strata? Why is this question important and interesting? This question is important for the following reasons: 1. Could tell us more about the environmental conditions in the poles and their effects on geologic features. 2. Could tell us which land cover is more likely to preserve signs of past/ present water. List any hypotheses you may have had of what the answer(s) might be to your science question. 1. Craters found on the polar ice caps will be more likely to be destroyed or modified due to the erosional forces of the ice primarily through frost action and basal slip. II. Background Depressions in the This image was collected February 29, 2004 during the end of southern summer season. ice surface caused The local time at the location of the image was about 2 pm. The image shows an area in by sub‐ice craters the South Polar Region. Seasonal changes. The planet's rotation axis is tilted with respect to the orbital plane by almost 24 degrees, so Mars does experience significant seasonal differences in the amount of sunlight falling on a hemisphere during a year. The difference between winter and summer is more extreme on Mars than on Earth, due to the greater eccentricity of the Martian orbit. The Red Planet receives 40 percent more sunlight during its southern summer, when nearest the Sun, than during its southern winter, when the Sun is most distant. -
Lunar and Planetary Science XXXI 1276.Pdf
Lunar and Planetary Science XXXI 1276.pdf THE FATE OF SALT ON MARS : GLOBAL EVIDENCE FOR A NORTHWARD OPEN SALT CYCLE R. D. Lorenz and R. A. Beyer, Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092, USA ([email protected]). Introduction: The general topographic gradient be- ducting a single deposition-dessication cycle, it is more tween the south and north, and the likelihood that likely that the water were cycled through the rocks of oceans on the Martian surface would have been ice- the south several times, leaching out soluble comp o- covered, suggests that the ancient Martian hydrologi- nents each time. Thus the 60m does not indicate an cal cycle had a largely noncycled involatile component upper limit. – salt. It seems likely that massive salt deposits may It is of course likely, especially in such a flood- exist in the low-lying regions of the north and in the ing/dessication cycle, that minerals would be deposited floor of Valles Marineris. in less extensive, but thicker, deposits corresponding Paradigm: Clifford and Parker [1,2] have con- to topographic lows in the surface/groundwater sys- structed a model of Martian hydrology. In particular, tem. they suggest that as the planet cooled, the cryosphere Evidence: Remote sensing evidence exists for would propagate downwards, sealing the aquifer in the evaporite deposits in general (e.g. the ‘White Rock’ [7]) south and freezing over any ocean. The ice-covered and more recently for possible salt domes themselves ocean (for which abundant – albeit largely circumstan- in the floor of Valles Marineris (Beyer et al., this con- tial - evidence now exists [3]) would slowly dry out, the ference) Here we discuss various effects that might be ice being sublimed and deposited on the ice caps. -
Copyrighted Material
1 Geological t ime 1.1 Introduction Why is geological time so important? It underpins everything we study in geology and Earth Science today and provides a framework for many other sciences. The age of the Earth and length of geological time have probably occupied human thought ever since we became conscious of our surround- ings. For centuries, people have attempted to quantify and measure it with varying degrees of success. With a signifi cant degree of certainty, we can now say that the Earth is around 4.65 billion years old, a fi gure that is, to most people, unimaginably long. Many “ creation science ” articles and books that talk about creationist stratigraphy, repeatedly claim that we use and misuse – in their view – geological time. So, is our perception of geology, Earth Science, the rock record, and geological time wrong? Perception of time has changed signifi cantly throughout history, depending on a variety of factors. Some of these will become apparent in the following chapters. When we look at much of the controversy that surrounds geology and other sciences, we fi nd that the perception and determination of time is frequently at the heart of the problem. However, why should this be an issue? The amount of time available for something to occur usually increases the possibility of it happening or the frequency at which it can take place. If time scales are short, changes and variations become more important; but as time scales increase, it is possible for the unusual to become, if not the norm, at least unexceptional. -
Multi-Model Meteorological and Aeolian Predictions for Mars 2020 and the Jezero Crater Region
Space Sci Rev (2021) 217:20 https://doi.org/10.1007/s11214-020-00788-2 Multi-model Meteorological and Aeolian Predictions for Mars 2020 and the Jezero Crater Region C.E. Newman1 · M. de la Torre Juárez2 · J. Pla-García3,4 · R.J. Wilson5 · S.R. Lewis6 · L. Neary7 · M.A. Kahre5 · F. Forget 8 · A. Spiga8,9 · M.I. Richardson1 · F. Daerden7 · T. Bertrand10,5 · D. Viúdez-Moreiras3 · R. Sullivan11 · A. Sánchez-Lavega12 · B. Chide13 · J.A. Rodriguez-Manfredi3 Received: 20 May 2020 / Accepted: 26 December 2020 / Published online: 8 February 2021 © The Author(s) 2021 Abstract Nine simulations are used to predict the meteorology and aeolian activity of the Mars 2020 landing site region. Predicted seasonal variations of pressure and surface and atmospheric temperature generally agree. Minimum and maximum pressure is predicted at Ls ∼ 145◦ and 250◦, respectively. Maximum and minimum surface and atmospheric tem- perature are predicted at Ls ∼ 180◦ and 270◦, respectively; i.e., are warmest at northern fall The Mars 2020 Mission Edited by Kenneth A. Farley, Kenneth H. Williford and Kathryn M. Stack Supplementary Information The online version contains supplementary material available at https://doi.org/10.1007/s11214-020-00788-2. B C.E. Newman [email protected] 1 Aeolis Research, Tucson, AZ, USA 2 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91001, USA 3 Centro de Astrobiología (CSIC-INTA), 28850 Madrid, Spain 4 Space Science Institute, Boulder, CO 80301, USA 5 Ames Research Center, Mountain View, CA, USA 6 The Open -
Topographic Map of Mars
U.S. DEPARTMENT OF THE INTERIOR OPEN-FILE REPORT 02-282 U.S. GEOLOGICAL SURVEY Prepared for the NATIONAL AERONAUTICS AND SPACE ADMINISTRATION 180° 0° 55° –55° Russell Stokes 150°E NOACHIS 30°E 210°W 330°W 210°E NOTES ON BASE smooth global color look-up table. Note that the chosen color scheme simply 330°E Darwin 150°W This map is based on data from the Mars Orbiter Laser Altimeter (MOLA) 30°W — 60° represents elevation changes and is not intended to imply anything about –60° Chalcoporous v (Smith and others 2001), an instrument on NASA’s Mars Global Surveyor Milankovic surface characteristics (e.g. past or current presence of water or ice). These two (MGS) spacecraft (Albee and others 2001). The image used for the base of this files were then merged and scaled to 1:25 million for the Mercator portion and Rupes map represents more than 600 million measurements gathered between 1999 1:15,196,708 for the two Polar Stereographic portions, with a resolution of 300 and 2001, adjusted for consistency (Neumann and others 2001 and 2002) and S dots per inch. The projections have a common scale of 1:13,923,113 at ±56° TIA E T converted to planetary radii. These have been converted to elevations above the latitude. N S B LANI O A O areoid as determined from a martian gravity field solution GMM2 (Lemoine Wegener a R M S s T u and others 2001), truncated to degree and order 50, and oriented according to IS s NOMENCLATURE y I E t e M i current standards (see below). -
Harborgracestandard18860109.Pdf
I HARBOR GRACE, NEWFOUDLAND, :JJATURDAY, JANUARY 9, 1886. VOLUJIIE.. XXVI . .. Adv_,rtisements. Miscellaneous. Items. -1'n& Naw Bttmsn Boan.-Tb.. totl\1 Xr 0 1&41\one'a plan ot H~ Bul• to Ad.Aert.isements. Advertisements. nou1ber or mtmben in the new Rritlth be KocUa.d.-Wha~ Be hopea to ~'~-------------~~~~ Itollie of COCIIOIODI will be 670, dinrlbat. The O~hoWlde of t.he AtlaDUo. TilE IIUSEST FAnliElL .t.chi•••· A acepllc.'l fl\r roor Aend:t the follo .. in~; 1- od ulollowa: ST. JOHN'S PH<ENIX Anol now t it~ hooet\L former pow l:.. un- Bor- Uoi.er· To- Londt11t, Dtc. 22 -It It glrt11 oal byltf. i1 ll queation --whether ·tb o ntl11' claa of h II Ill • I•P"" lor I no to"": tiea. ouahl. aitlu. tala. Gladttone'e intimates tba* l.be plu Df at-thipe or utromc •s-<1 ""d enormoua Marble & Freestone Wo1ks Fire Assurance Company. Tltl4 Ia lbot.ov row I" t.b• u t'k•- England...... m~ol 2:l6 6 465 Home RuJe wllleb he •Ill aetaally lnUo tlu CllD be fUado 1\8 •cceptAllle to thlro own· 0 0 0 Wain....... .... 19 ll so duee loto l'ullameul will be a nry muth era •• .to the public, for 'he IMJiil upe~ooe Anll lltl~ ltlowor doWll- 89 Sl 1 12 leae formidable scheme t han t.bM 111hillh ALEXA~OElt s~uTn. PIIOI'RIETOR. LCl: DAnn 8TBEE1' It: COABI!SCi CflOllS Scotll\ntl ......... for tlrat con Rnd tnA1~n11nce mAiccs it 0 0 ~ 0 0 0 0 Jrel1111d .......... -
Integrated Geoscientific Interpretation and 3D Modelling of a Proterozoic
Solid Earth, 11, 1053–1077, 2020 https://doi.org/10.5194/se-11-1053-2020 © Author(s) 2020. This work is distributed under the Creative Commons Attribution 4.0 License. Mapping undercover: integrated geoscientific interpretation and 3D modelling of a Proterozoic basin Mark D. Lindsay1, Sandra Occhipinti1,2, Crystal Laflamme1,3, Alan Aitken1, and Lara Ramos1 1The Centre for Exploration Targeting, School of Earth Sciences, The University of Western Australia, Crawley, Western Australia, 6009, Australia 2Mineral Resources, Commonwealth Science and Industry Research Organisation, Kensington, Western Australia, 6151, Australia 3Department of Geology and Geological Engineering, Laval University, Québec City, Québec G1V 0A6, Canada Correspondence: Mark D. Lindsay ([email protected], [email protected]) Received: 4 December 2019 – Discussion started: 17 January 2020 Revised: 29 April 2020 – Accepted: 15 May 2020 – Published: 24 June 2020 Abstract. Gravity and 3D modelling combined with geo- Bryah sub-basin and Padbury Basin. The conclusion is that chemical analysis examine the subsurface within and below the formation of the Yerrida Basin involves a geodynamic the poorly exposed Palaeoproterozoic Yerrida Basin in cen- history more complex than previously thought. This result tral Western Australia. Understanding the structure of a re- highlights the value in geophysics and geochemistry in re- gion is important as key features indicating past geodynamic vealing the complexity of the earlier geodynamic evolution processes and tectonic activity can be revealed. However, in of the basin that may be indiscernible from surface geology stable, post-depositional tectonic settings only the younger but may have high importance for the tectonic development sedimentary units tend to be widely exposed, rendering di- of the region and its mineral resources. -
International Commission on the History of Geological Sciences
International Commission on the History of Geological Sciences INHIGEO ANNUAL RECORD No. 50 Covering Activities generally in 2017 Issued in 2018 INHIGEO is A Commission of the International Union of Geological Sciences & An affiliate of the International Union of the History and Philosophy of Science and Technology Compiled and Edited by William R. Brice INHIGEO Editor Printed in Johnstown, Pennsylvania, USA, on request Available at www.inhigeo.com ISSN 1028-1533 1 2 CONTENTS INHIGEO Annual Record No. 50 (Published in August 2018 and covering events generally in 2017) INHIGEO BOARD………………………………………………………………………..…………..…..6 MESSAGES TO MEMBERS President’s Message: Barry Cooper..……………………………………………………….…….7 Secretary-General’s Report: Marianne Klemun...……………………………………………......8 Editor’s Message: William R. Brice…………………………………………………………….10 INHIGEO CONFERENCE REPORT INHIGEO Conference, Yerevan, Armenia 12 to 18 September 2017……………………………………………….…………….….12 "Personalities of the INHIGEO: From Madrid (2010) To Cape Town (2016)" By L. Kolbantsey and Z. Bessudnova…………………………………...……………....29 INHIGEO CONFERENCES 43rd Symposium – Mexico City, 12-21 November 2018………………………………………...35 Future Scheduled conferences………….…………………………………..……………………36 44th INHIGEO Symposium, Varese and Como (Italy), 2-12 September 2019………….36 45th INHIGEO Symposium – New Delhi, India, 2020……………...…………………..37 46th INHIGEO Symposium – Poland, 2021……………………………………………..37 OTHER CONFERENCES Symposium on the Birth of Geology in Argentinean Universities………...………………….…37 Austrian Working Group -
Colonization: a Permanent Habitat for the Colonization of Mars
COLONIZATION A PERMANENT HABITAT FOR THE COLONIZATION OF MARS A thesis submitted in fulfilment of the requirements of the degree of Master in Engineering Science (Research) in Mechanical Engineering BY MATTHEW HENDER THE UNIVERSITY OF AD ELAIDE SCHOOL OF MECHANICAL ENGINEERING SUPERVISOR S – DR. GERALD SCHNEIDER & COLIN HANSEN A u g u s t 2 0 0 9 315°E (45°W) 320°E (40°W) 325°E (35°W) 330°E (30°W) 335°E (25°W) 340°E (20°W) 345°E (15°W) 350°E (10°W) 355°E (5°W) 360°E (0°W) 0° 0° HYDRAOTES CHAOS . llis Dia-Cau Va vi Ra . Camiling Aromatum Chaos . Rypin Chimbote . Mega . IANI MERIDIANI PLANUM* . v Wicklow Windfall Zulanka Pinglo . Oglala Tuskegee . Bamba . CHAOS . Bahn . Locana. Tarata . Spry Manti Balboa ARABIA Huancayo . AUREUM . Groves . Vaals . Conches _ . Sitka Berseba . Kaid . Chinju Lachute . Manah Rakke CHAOS . Stobs . Byske -5° . Airy-0 . -5° Butte. Azusa Kong Timbuktu . Quorn Airy . Creel . Innsbruck XANTHE Wink TERRA TERRA A . Kholm M . Daet S A Ganges .Sfax . Paks H Batoka C Chasma . Rincon I Arsinoes . Glide R P AURORAE CHAOS A Chaos C I S E R M R I N A E R R F G A I T I A R -10° -10° M Pyrrhae C H A O S S Chaos E L L A V MARGARITIFER Eos Mensa* EOS CHASMA Beer -15° -15° alles V L o i r e Osuga Eos TERRA Chaos V a Jones l l e s Vinogradov -20° Lorica Polotsk -20° s Sigli . Kimry . Lebu Valle S Kansk .