Author Indexl

Total Page:16

File Type:pdf, Size:1020Kb

Author Indexl Author Indexl Adams, L. H. 58, 186 De Sitter, L. U. 237, 238, 242 Aki, K. 228 Deuker, E. A. 67, 69 Allan, D. W. 55, 58 Deutsch, E. R 61 Anderson, E. M. 221, 243 Dietrich, G. 249 Arrhenius, S. 259 Dobrin, M. B. 259, 260, 261 Du Toit, A. L. 6, 7, 8, 9, 180 Baker, H. B. 6, 7 Baldwin, R B. 251, 252 Eckart, C. 67 Barrell, J. 265 Egyed, L. 11, 205 Barringer, D. M. 24 Elkins, T. A. 241 Basset, A. B. 149 Eotvos, Rv. 119 Beals, C. S. 24 Epstein, P. S. 119 Belousov, V. V. 196, 204, 242 Ertel, H. 119, 120 Bemmelen, H. W. van 196, 198 Escher, B. G. 140 Benioff, H. 39, 40, 41, 106, 108, 109, 111 Ewing, M. 19, 76 Berlage, H. P. 196, 198 Ez, V. V. 242 Bijlaard, P. P. 83, 248 Birch, F. 55, 62, 139, 172 Fairbairn, H. W. 105 Bondi, H. 107 Farquhar, R M. 52, 53, 54 Bowden, F. P. 232 Ferguson, G. M. 24 Bowie, W. 140 Fisher, O. 140 Bridgman, P. W. 105 Brock, B. B. 20 Garland, G. D. 31 Brooks, H. 191 Geszti, J. 247 Bucher, W. H. 143, 167 Gilman, J. J. 99, 100 Bullard, E. C. 56 Goguel, J. 124, 125 Bullen, K. E. 49, 50, 51, 104 Gold, T. 107, 126, 127 Byerly, P. 43 Graham, J. W. 61 Graton, L. C. 263 Carey, S. W. 248 Green, A. E. 69 Chandrasekhar, S. 135, 152, 187 Griffith, A. A. 98, 99 Chen, C. H. 242 Griffiths, D. H. 61 Chertkova, E. I. 242 Griggs, D. 105, 132, 187, 188, 190 Clegg, J. A. 61 Gurevich, G. I. 256 Cloos, E. 256 Gutenberg, B. 28, 29, 32, 35, 36, 37, 38, -,H. 242 39,48,49,50,56,106,108,111,129,142 GzovskiI, M. V. 261 Daly, R. A. 265 Darwin, G. H. 126, 140 Haarmann, E. 141, 196 Davison, C. 153, 166 Hafner, W. 223 De Geer, C. J. 29 Handin, J. 105 1 Slavonic names have been transliterated according to the Cambridge system; this is the system used, for instance, in Physics Abstracts. Author Index 273 Haskell, N. A. 111, 266 Labrouste, H. 49 Havemann, H. 198 Lake, P. 13 Heaps, H. S. 265 Lamb, H. 85, 147, 162, 257 Heezen, B. C. 19 Lambert, W.D. 119, 126 Heim, A. 15 Landau, A. 24 Heiskanen, W. 31 Lebedev, V. 1. 206 Hencky, H. 83 Lee, J. S. 242 Hersey, M. D. 91 -,M. T. 242 Hess, H. H. 191, 192 Lees, G. M. 63 Heywood, W. W. 26 Leutert, W. 154 Hiersemann, L. 35, 36 Lohest, M. 25 Hill, M. J. 20 Love, A. E. H. 74 -, R. 80 Low, A. R. 87 Hills, G. F. S. 144 Lyustikh, E. N. 111, 265 Hirschmann, J. 19 Hobbs, W. H. 20 Malinovskaya, L. N. 231 Hodgson, J. H. 45 Marble, J. P. 4 Holmes, A. 3, 23, 186 Mason, B. 62 Honda, H. 47 Matschinski, M. 155, 192, 205 Hopkins, W. 186 Matuzawa, T. 226 Housner, G. W. 234 McAdams, W. H. 87 Hoyle, F. 136, 138 McDowell, A. N. 261 Hubbert, M. K. 240, 242 Melchior, P. J. 108 Milankovitch, M. 117, 119, 127, 129, 130, Inglis, C. E. 76, 99 131, 208 -, D. R. 125 Milverton, S. W. 87 Mintrop, L. 48 Jacobs, J. A. 56, 57, 58, 139 Mises, R. v. 80 Jaeger, J. C. 74 Mohr, O. 70, 93 Jaggar, T. A. 27 Mollard, J. R. 23 Jardetzky, W. S. 76, 193, 245 Moody, J. D. 20 Jeffreys, H. 74, 86, 106, 107, 110, 116. Mott, N. F. 99 126, 132, 133, 136, 141, 163, 167, Munk, W. H. 126 168 Jobert, G. 132 Nadai, A. 83, 132 Johnston, W. A. 265 Nakano, H. 231 Joksch, H.C. 9,10,157 Nettleton, L. L. 241, 259, 261 Jordan, P. 157 Neumayr, M. 2, 27, 34 Jung, K. 116 Nininger, H. H. 24 Niskanen, E. 265, 270 Kaariiiinen, E. 29 Kalle, K. 249 Kampe de Feriet, J. 184 Oldroyd, J. G. 68, 71, 91 Kawasumi, H. 43 bpik, E. 253 KeIlis-Borok, V. I. 43 Orowan, E. 93, 94, 95, 96, 97, 98, 99 Kogan, S. D. 35, 37 Koppen, W. 4, 5, 9 Pai, S. 184 Kosminskaya, I. P. 49 Pekeris, C. L. 148, 149, 187 Kossinna, E. 9, 10 Pellew, A. 87 Kreichgauer, D. 4, 5 Petch, N. J. 98 Kuenen, P. H. 242 Pirson, L. V. 14 Kuiper, G. P. 136 Press, F. 47, 76 Kukkamaki, T. J. 29 Prey, A. 123 Scheidegger, Principles of Geodynamics 18 274 Author Index Quiring. H. L. 140 Southwell. R. V. 87 Stille. H. 12 Ramberg. H. 25. 256. 257 Strakhov. N. M. 11 Ramsey. W. H. 62 Suess. F. E. 2. 27. 34 Rankama. K. 61 Reiner. M. 87. 88. 89. 90 Tabor. D. 232 Reuss. A. 81 Terzaghi. K. 112 Richter. C. F. 32. 35. 36. 37. 38. 39. 108 Tiedemann. A. W. 238. 239 Riedel. W. 242 Travis. J. P. 261 Rittmann. A. 264 Truesdell. C. 65. 69 Riznichenko. Yu. V. 49 Tsuboi. C. 32. 33. 56 Roberts. D. K. 100 Turner. F. J. 105 Robertson. E. C. 105 Robinson. R. O. A. 172 Umbgrove. J. H. F. 12. 13 Robson. G. R. 56 Urey. H. C. 152 RotM. J. P. 49 Urry. W. D. 139 Rudnik. P. 107 Runcorn. S. K. 60. 61 Veitsman. P. S. 49 Russell. R. D. 52. 53. 54 Vening Meinesz. F.A. 20. 111.145.189. Rutten. L. M. R. 12 208. 210. 211. 212 Ruud. 1. 165. 247 Verhoogen. J. 56. 57. 263. 264 Vvedenskaya. V. V. 232 Sahama. T. G. 61 Sapper. K. 143 Walker. A. M. 107 Saunders. O. A. 87 Wegener. A. 4. 5. 7. 142. 180. 181 Sauramo. M. 29. 265 Wegmann. C. E. 256 Scheidegger. A. E. 13. 21. 23. 24. 41. 42. Weizsacker. C. F. v. 135 43. 44. 65. 72. 86. 90. 102. 120. 146. Wells. A. A. 100 153. 165. 168. 170. 172. 183. 270 Willmore. P. L. 24. 56 Schmidt. E. R. 208 Wilson. J. T. 13. 15. 16. 17. 18. 19. 52. -.R.J.87 53. 54. 143. 164. 165. 166 Schuchert. C. 15 Woolnough. W. G. 153 Schulz-Weidner. W. 24 Worzel. J. L. 48 Shurbet. G. L. 48 Wylie. C. C. 255 Skerl. J. G. A. 7 Slichter. L. B. 58 Young. A. 107 Smart. W. M. 135 Sonder. R. A. 23. 167. 172 Zardecki see J ardetzky Sorskil. A. A. 258 Zerna. W. 69 Sotome. K. 193 Zoelly. R. 154 Subject Index Additional stress definition Arctic piercement domes 26 Bulk modulus (incompressi­ 72ff. Argon (radiogenic) 52 bility) 74 - - in Earth 223 Arizona crater, origin 253, Buoyancy (of domes) 260 Africa, heat flow 55 255 -, paleoclimate 4 - -, physiography 24, 25 Calcium (radiogenic) 52 -, rift valleys 19, 33, 249 Asia, island arcs 14, 15, 16 California, earthquakes in After-effect (elastic) 89 -, mountain roots in 49 38 Aftershocks (in earth- Atlantic Ocean, heat flow 55 -, mountain roots 49 quakes) 108ff. -, origin of (zonal ro- Canada, heat flow 55 Age, determination 51 tation) 193 -, line patterns 23 -, of geological epochs 4 -, physiography 6, 48 Canadian shield 53f£' Airy function 74 -, ridges 19 Cap range, description 16 Airy hypothesis 31, 49 -, spreading theory 142 -, theory 174, 177 Alaska (mountains) 13 Autocorrelation 184 Carlsberg ridge 19 Aleutians 13, 14, 15, 37 Auxiliary plane 22, 43, 229 Cataclysmic theory of origin Alpine cycle 12 Axis (of fold) 23 of earth 136 Alps, nappes 23 Catastrophe in mountain -, physiography 16 Bands of instability 113 building 12 -, roots 48, 49 Barringer crater (see Ari- Cauchy-Riemann equations -, shortening 15 zona crater) 80 -, speed of formation 162 Basalt, description 63 Chandler wobble 107 Altitude effect (on gravity) -, origin of 144 Circulations, definition 84 30 -, quantity in crust 143 -, on Earth 124ff. America, drift of 184 Basaltic layer 49 Classical bodies 87 -, origin of 194 Batholith 3 ClausiUS-Clapeyron equa- -, paleoclimate 4 BIJLAARD'S theory 113, 213, tion 227 -, westward motion 132, 217, 248 Climate (ancient) 4 184 Bingham solid 90 Coast Range 15, 16 Anatexis 63 Birch discontinuity 50, 62, Cohesion (molecular) 97 ANDERSON'S theory 221 ff., 186, 198, 220 Compatibility condition 67 243 Boudinage, description 25 ff. Competent layer 25, 256ff. Andes 14, 16 -, theory 256f£' Compressional waves, de- Andesite, description 63 Bouguer anomaly 31 finition 33 -, origin 144 Branch point line 165, 247 -, see also P waves -, quantity in crust 143 Brasil, paleoclimate 4 Concentric folding 237ff. -, line 63 Britain, heat flow 55 Congo: volcanoes 28 Anomalies (gravity) 30 British Columbia, mountain Conrad discontinuity 49 Antarctica (uplift) 265 ranges 13 Conservation of phase signs Anticline 23 Brittleness 93 42 Appalachian cycle 12 -, in notches 94 Constitutive equations 71 Appalachians 15 -, see also fracture, brittle Continental drift, concept Archean rocks 53, 258 Buckling, description 79 6ff. Arcs (mountain and island) -, in orogenesis 175, 205, -, magnetic evidence 61 35 (see also orogenesis) 236 -, theory 141 ff., 179ff. 18* 276 Subject Index Continents, crustal studies Damping of oscillations 89 Elastic constants of Earth 47 Dating, paleontological 3 104ff. -, dynamics 134ff. Dating, radioactive 51 ff Elastic limit 80 -, geography 6 Deep earthquakes 35 Elasticity theory 73 ft. -, growth theory 53ff., Deflections 16 Ellipticity of Earth 116 143ff., 166 Deformation, description 65 Energy of earthquake -, margin 33 -, measure 65 38ff. -, nucleus 53 -, mechanics 64ff. Epicenter 33 -, spreading 142 Density, definition 67 Equation of motion 69 Continuity condition 68ff. -, Earth 30, 50ff. Europe: paleoclimate 4 Continuous media 64 Depth of focus 35 Evolution (geological) 2 Contraction theory 144, Detrition 3 Expansion theory 154, 162ff.
Recommended publications
  • Planetary Surfaces
    Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I].
    [Show full text]
  • Martian Crater Morphology
    ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter.
    [Show full text]
  • Earth: Atmospheric Evolution of a Habitable Planet
    Earth: Atmospheric Evolution of a Habitable Planet Stephanie L. Olson1,2*, Edward W. Schwieterman1,2, Christopher T. Reinhard1,3, Timothy W. Lyons1,2 1NASA Astrobiology Institute Alternative Earth’s Team 2Department of Earth Sciences, University of California, Riverside 3School of Earth and Atmospheric Science, Georgia Institute of Technology *Correspondence: [email protected] Table of Contents 1. Introduction ............................................................................................................................ 2 2. Oxygen and biological innovation .................................................................................... 3 2.1. Oxygenic photosynthesis on the early Earth .......................................................... 4 2.2. The Great Oxidation Event ......................................................................................... 6 2.3. Oxygen during Earth’s middle chapter ..................................................................... 7 2.4. Neoproterozoic oxygen dynamics and the rise of animals .................................. 9 2.5. Continued oxygen evolution in the Phanerozoic.................................................. 11 3. Carbon dioxide, climate regulation, and enduring habitability ................................. 12 3.1. The faint young Sun paradox ................................................................................... 12 3.2. The silicate weathering thermostat ......................................................................... 12 3.3. Geological
    [Show full text]
  • Origin of the Solar System
    Creation Myths The rise of the monotheistic religions changed this view. When one of the gods got a higher Old Myths status than others (who in some cases became Speculation about the origin and evolution of demons or devils), he continued to increase in the earth and the celestial bodies is probably as prestige and power until he became the Supreme old as human thinking. During the millennia that Lord, the undisputed ruler of the whole world. are covered by the history of science, philosphy, Then it was not enough for him to create the world and religion we can distinguish three types of ap­ in the sense of organizing a preexisting chaos; he proach to this problem. had to create it all from nothing (ex nihilo) by The first is the "theocratic-myth" approach, pronouncing a magic word or by his will power. according to which the evolution of the world was This is the meaning of "creation" when we use it governed by gods who once upon a time created today, but it is a relatively new concept. It was it. However, we must remember that the meaning generally accepted in Christianity in the second of "creation" has changed. The earliest meaning century A.D. but the Genesis description of the of this term seems to have been that the gods Creation seems to have either meaning. The crea­ brought order into a preexisting chaos. The world tion ex nihilo was not generally accepted by the was "ungenerated and indestructible"-as Aris­ philosophical-scientific community until the syn­ totle puts it-and the gods were part of this world thesis by St.
    [Show full text]
  • 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
    [Show full text]
  • Supporting Information (SI) Appendix Persistence and Origin of the Lunar Core Dynamo
    Supporting Information Corrected July 05, 2013 Supporting Information (SI) Appendix Persistence and origin of the lunar core dynamo Clément Suavet, Benjamin P. Weiss, William S. Cassata, David L. Shuster, Jérôme Gattacceca, Lindsey Chan, Ian Garrick-Bethell, James W. Head, Timothy L. Grove, and Michael D. Fuller 1. Previous paleomagnetic studies of high-K mare basalts During the Apollo era, paleomagnetic studies were carried out on at least six high-K basalts: 10017, 10022, 10024, 10049, 10057, and 10069. 10022 was thermally demagnetized (49), but the lack of published directional data precludes the identification of magnetization components. 10024 was found to carry an intense soft overprint and a higher coercivity component blocked from 5 to at least 50 mT, but spurious demagnetization effects prevented a detailed characterization of the latter (1). Similarly, 10057 was found to contain a soft overprint and a higher coercivity component from 9 to >18 mT, but a high-quality paleointensity value could not be obtained because the sample was not fully demagnetized (50, 51). 10069 was only demagnetized to <7 mT before thermal demagnetization was attempted, at which point the sample irreversibly altered (49). Because so many lunar rocks have poor magnetic recording properties (52), we decided to focus on two samples that appeared to be unusually well-behaved during previous AF demagnetization experiments: 10017 and 10049 (Fig. S1 and Table S6). The natural remanent magnetization (NRM) of 10017 was studied by three groups (13-16). Initial reports identified a directionally stable magnetization component during alternating field (AF) demagnetization of subsample 10017,64 up to 50 mT (13).
    [Show full text]
  • Climate Change and Freshwater Fisheries
    See discussions, stats, and author profiles for this publication at: https://www.researchgate.net/publication/282814011 Climate change and freshwater fisheries Chapter · September 2015 DOI: 10.1002/9781118394380.ch50 CITATIONS READS 15 1,011 1 author: Chris Harrod University of Antofagasta 203 PUBLICATIONS 2,695 CITATIONS SEE PROFILE Some of the authors of this publication are also working on these related projects: "Characterizing the Ecological Niche of Native Cockroaches in a Chilean biodiversity hotspot: diet and plant-insect associations" National Geographic Research and Exploration GRANT #WW-061R-17 View project Effects of seasonal and monthly hypoxic oscillations on seabed biota: evaluating relationships between taxonomical and functional diversity and changes on trophic structure of macrobenthic assemblages View project All content following this page was uploaded by Chris Harrod on 28 February 2018. The user has requested enhancement of the downloaded file. Chapter 7.3 Climate change and freshwater fisheries Chris Harrod Instituto de Ciencias Naturales Alexander Von Humboldt, Universidad de Antofagasta, Antofagasta, Chile Abstract: Climate change is among the most serious environmental challenge facing humanity and the ecosystems that provide the goods and services on which it relies. Climate change has had a major historical influence on global biodiversity and will continue to impact the structure and function of natural ecosystems, including the provision of natural services such as fisheries. Freshwater fishery professionals (e.g. fishery managers, fish biologists, fishery scientists and fishers) need to be informed regarding the likely impacts of climate change. Written for such an audience, this chapter reviews the drivers of climatic change and the means by which its impacts are predicted.
    [Show full text]
  • Who Got Moseley's Prize?
    Chapter 4 Who Got Moseley’s Prize? Virginia Trimble1 and Vera V. Mainz*,2 1Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, United States 2Department of Chemistry, University of Illinois at Urbana-Champaign, Urbana, Illinois 61802, United States *E-mail: [email protected]. Henry Gwyn Jeffreys Moseley (1887-1915) made prompt and very skilled use of the then new technique of X-ray scattering by crystals (Bragg scattering) to solve several problems about the periodic table and atoms. He was nominated for both the chemistry and physics Nobel Prizes by Svante Arrhenius in 1915, but was dead at Gallipoli before the committees finished their deliberations. Instead, the 1917 physics prize (announced in 1918 and presented on 6 June 1920) went to Charles Glover Barkla (1877-1944) “for discovery of the Röntgen radiation of the elements.” This, and his discovery of X-ray polarization, were done with earlier techniques that he never gave up. Moseley’s contemporaries and later historians of science have written that he would have gone on to other major achievements and a Nobel Prize if he had lived. In contrast, after about 1916, Barkla moved well outside the scientific mainstream, clinging to upgrades of his older methods, denying the significance of the Bohr atom and quantization, and continuing to report evidence for what he called the J phenomenon. This chapter addresses the lives and scientific endeavors of Moseley and Barkla, something about the context in which they worked and their connections with other scientists, contemporary, earlier, and later. © 2017 American Chemical Society Introduction Henry Moseley’s (Figure 1) academic credentials consisted of a 1910 Oxford BA with first-class honors in Mathematical Moderations and a second in Natural Sciences (physics) and the MA that followed more or less automatically a few years later.
    [Show full text]
  • Special Regions’’: Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2)
    ASTROBIOLOGY Volume 14, Number 11, 2014 News & Views ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2014.1227 A New Analysis of Mars ‘‘Special Regions’’: Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2) John D. Rummel,1 David W. Beaty,2 Melissa A. Jones,2 Corien Bakermans,3 Nadine G. Barlow,4 Penelope J. Boston,5 Vincent F. Chevrier,6 Benton C. Clark,7 Jean-Pierre P. de Vera,8 Raina V. Gough,9 John E. Hallsworth,10 James W. Head,11 Victoria J. Hipkin,12 Thomas L. Kieft,5 Alfred S. McEwen,13 Michael T. Mellon,14 Jill A. Mikucki,15 Wayne L. Nicholson,16 Christopher R. Omelon,17 Ronald Peterson,18 Eric E. Roden,19 Barbara Sherwood Lollar,20 Kenneth L. Tanaka,21 Donna Viola,13 and James J. Wray22 Abstract A committee of the Mars Exploration Program Analysis Group (MEPAG) has reviewed and updated the description of Special Regions on Mars as places where terrestrial organisms might replicate (per the COSPAR Planetary Protection Policy). This review and update was conducted by an international team (SR-SAG2) drawn from both the biological science and Mars exploration communities, focused on understanding when and where Special Regions could occur. The study applied recently available data about martian environments and about terrestrial organisms, building on a previous analysis of Mars Special Regions (2006) undertaken by a similar team. Since then, a new body of highly relevant information has been generated from the Mars Reconnaissance Orbiter (launched in 2005) and Phoenix (2007) and data from Mars Express and the twin Mars Exploration Rovers (all 2003).
    [Show full text]
  • Impact Cratering – Fundamental Process in Geoscience and Planetary Science
    Impact cratering – fundamental process in geoscience and planetary science JKPati1 and WUReimold2 1Department of Earth and Planetary Sciences, Nehru Science Centre, University of Allahabad, Allahabad 211 002, India. e-mail: [email protected] 2Museum f. Natural History (Mineralogy), Humboldt-University in Berlin, Invalidenstrasse 43, D-10115 Berlin, Germany. e-mail: [email protected] Impact cratering is a geological process characterized by ultra-fast strain rates, which generates extreme shock pressure and shock temperature conditions on and just below planetary surfaces. Despite initial skepticism, this catastrophic process has now been widely accepted by geoscientists with respect to its importance in terrestrial – indeed, in planetary – evolution. About 170 impact structures have been discovered on Earth so far, and some more structures are considered to be of possible impact origin. One major extinction event, at the Cretaceous–Paleogene boundary, has been firmly linked with catastrophic impact, but whether other important extinction events in Earth history, including the so-called “Mother of All Mass Extinctions” at the Permian–Triassic boundary, were triggered by huge impact catastrophes is still hotly debated and a subject of ongoing research. There is a beneficial side to impact events as well, as some impact structures worldwide have been shown to contain significant (in some cases, world class) ore deposits, including the gold– uranium province of the Witwatersrand basin in South Africa, the enormous Ni and PGE deposits of the Sudbury structure in Canada, as well as important hydrocarbon resources, especially in North America. Impact cratering is not a process of the past, and it is mandatory to improve knowledge of the past-impact record on Earth to better constrain the probability of such events in the future.
    [Show full text]
  • Revised Summary of Apollo Drive Tubes
    Revised Summary of Apollo Drive Tubes Figure 1: Photo of double drive tube at Apollo 14. NASA photo AS14-68-9454. Foot prints and cart tracks visible. the continuous and random cratering of the lunar Introduction surface results in a fine-grained mixture of rock and In addition to 3 deep drill cores taken during Apollo fused soil fragments in a manner likened to “gardening” missions, as many as 21 shallow drive tubes were used (Shoemaker 1971; Arnold 1975). However, the drill to core the lunar surface regolith down to ~50 cm. cores and drive tubes did successfully record the profile Although it had been expected that there would be of cosmogenic radionuclides produced by solar and significant stratigraphy preserved in these cores, little galactic cosmic ray bombardment and the was found. When you think about it, you realize that corresponding neutron flux that extends with depth (1 Lunar Sample Compendium C Meyer 2007 Table 1. Apollo Drive Tubes (only). weight length station containers other date Newsletter grams cm. bag ALSRC dissected # 10004 S 44.8 13.5 LM yes 23 grams biology 1978 10005 S 53.4 10 LM yes 27 grams biology 1978 12026 S 101.4 19.3 Surveyor Crater yes leaked, spilled, 47 g. bio. 12027 S 80 17.4 Sharp Crater yes leaked 1979 26 12028 U 189.6 31.6 Halo Crater yes leaked, compounded, 10 g. bio. 1970 12025 L 56.1 9.5 Halo Crater yes leaked 14220 S 80.7 16.5 G, near LM yes 1979 24 14230 S 76.7 12.5 North Triplet C.
    [Show full text]
  • 1982 L University of California San Diego -:-Ri Research Marine Physical Laboratory __~~
    Cover: Night aboard RIV Melville. Taken at 21°N during the Oasi s 82 expedition in the Pacific Ocean. CO VER BY l. D FORD DEDICATION In 1957 the eastern North Pacific Ocean was a few degrees warmer than normal. Weather patterns, sportfishing, and commercial fishing were affected, and oceanographers were puzzled. The late Professor John D. Isaacs called together a large group of scientists to talk about these remarkable conditions. Among those at the Rancho Santa Fe symposium in June 1958 was Dr. Jerome Namias. "It became apparent," he said later, " that the ocean contained the potential for affecting the weather substantially over vast areas." Dr. Namias has pursued the complex relationship between the oceans and the weather for many years. His long-range forecasts are front-page news . The vagaries of New England weather, as illustrated to him in Fall River, Massachusetts, piqued his boyhood curiosity. A stimulating high-school physics teacher and a scholarly amateur meteorologist encouraged his interest. The enthusiastic student set up his first weather station when he was sixteen. He went on to the Massachusetts Institute of Technology, where he participated with Carl Gustof Rossby Dr. Jerome Namias and Hurd C. Willett in a five-year effort to develop methods of long-range forecasting-an outgrowth of the Dust Bowl disaster of the 1930s. Bureau . His participation in forecasts for Atlantic convoys In 1941 Dr. Namias was called to Washington, D.C. to and Allied invasions led to his receiving a citation from the set up the Extended Forecast Section of the U.S.
    [Show full text]