Features Named After 07/15/2015) and the 2018 IAU GA (Features Named Before 01/24/2018)
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Ahuna Mons on Ceres 29 July 2019
Image: Ahuna Mons on Ceres 29 July 2019 More recently, a study of Dawn data led by ESA research fellow Ottaviano Ruesch and Antonio Genova (Sapienza Università di Roma), published in Nature Geoscience in June, suggests that a briny, muddy 'slurry' exists below Ceres' surface, surging upwards towards and through the crust to create Ahuna Mons. Another recent study, led by Javier Ruiz of Universidad Complutense de Madrid and published in Nature Astronomy in July, also indicates that the dwarf planet has a surprisingly dynamic geology. Ceres was also the focus of an earlier study by Credit: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA ESA's Herschel space observatory, which detected water vapour around the dwarf planet. Published in Nature in 2014, the result provided a strong indication that Ceres has ice on or near its surface. This image, based on observations from NASA's Dawn confirmed Ceres' icy crust via direct Dawn spacecraft, shows the largest mountain on observation in 2016, however, the contribution of the dwarf planet Ceres. the ice deposits to Ceres' exosphere turned out to be much lower than that inferred from the Herschel Dawn was the first mission to orbit an object in the observations. asteroid belt between Mars and Jupiter, and spent time at both large asteroid Vesta and dwarf planet The perspective view depicted in this image uses Ceres. Ceres is one of just five recognised dwarf enhanced-color combined images taken using blue planets in the Solar System (Pluto being another). (440 nm), green (750 nm), and infrared (960 nm) Dawn entered orbit around this rocky world on 6 filters, with a resolution of 35 m/pixel. -
The Parliament of Poets: an Epic Poem
The Parliament of Poets “Like a story around a campfire.” —From the Audience “A great epic poem of startling originality and universal significance, in every way partaking of the nature of world literature.” —Dr. Hans-George Ruprecht, CKCU Literary News, Carleton University, Ottawa, Canada “A remarkable poem by a uniquely inspired poet, taking us out of time into a new and unspoken consciousness...” —Kevin McGrath, Lowell House, South Asian Studies, Harvard University “Mr. Glaysher has written an epic poem of major importance... Truly a major accomplishment and contribution to American Letters... A landmark achievement.” —ML Liebler, Department of English, Wayne State University, Detroit, Michigan “Glaysher is really an epic poet and this is an epic poem! Glaysher has written a masterpiece...” —James Sale (UK), The Society of Classical Poets “And a fine major work it is.” —Arthur McMaster, Contributing Editor, Poets’ Quarterly; Department of English, Converse College, Spartanburg, South Carolina “This Great Poem promises to be the defining Epic of the Age and will be certain to endure for many Centuries. Frederick Glaysher uses his great Poetic and Literary Skills in an artistic way that is unique for our Era and the Years to come. I strongly recommend this book to all those who enjoy the finest Poetry. A profound spiritual message for humanity.” —Alan Jacobs, Poet Writer Author, Amazon UK Review, London “Very readable and intriguingly enjoyable. A masterpiece that will stand the test of time.” —Poetry Cornwall, No. 36, England, UK “Bravo to the Poet for this toilsome but brilliant endeavour.” —Umme Salma, Transnational Literature, Flinders University, Adelaide, Australia “Am in awe of its brilliance.. -
Constructing and Reconstructing Images of Chinese Women in Lin Yutang's Translations, Adaptations and Rewritings
CONSTRUCTING AND RECONSTRUCTING IMAGES OF CHINESE WOMEN IN LIN YUTANG'S TRANSLATIONS, ADAPTATIONS AND REWRITINGS by Fang Lu B.A., Beijing Normal University, 1987 M.A., Beijing Normal University, 1990 THESIS SUBMITTED IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY Under Special Arrangement Faculty of Arts & Social Sciences © Fang Lu 2008 SIMON FRASER UNIVERSITY Spring 2008 All rights reserved. This work may not be reproduced in whole or in part, by photocopy or other means, without permission of the author. Library and Bibliotheque et 1*1 Archives Canada Archives Canada Published Heritage Direction du Branch Patrimoine de I'edition 395 Wellington Street 395, rue Wellington Ottawa ON K1A0N4 Ottawa ON K1A0N4 Canada Canada Your file Votre reference ISBN: 978-0-494-46812-8 Our file Notre reference ISBN: 978-0-494-46812-8 NOTICE: AVIS: The author has granted a non L'auteur a accorde une licence non exclusive exclusive license allowing Library permettant a la Bibliotheque et Archives and Archives Canada to reproduce, Canada de reproduire, publier, archiver, publish, archive, preserve, conserve, sauvegarder, conserver, transmettre au public communicate to the public by par telecommunication ou par Plntemet, prefer, telecommunication or on the Internet, distribuer et vendre des theses partout dans loan, distribute and sell theses le monde, a des fins commerciales ou autres, worldwide, for commercial or non sur support microforme, papier, electronique commercial purposes, in microform, et/ou autres formats. paper, electronic and/or any other formats. The author retains copyright L'auteur conserve la propriete du droit d'auteur ownership and moral rights in et des droits moraux qui protege cette these. -
New Studies Provide Unexpected Insights Into Dwarf Planet Ceres 1 September 2016
New studies provide unexpected insights into dwarf planet Ceres 1 September 2016 Mons. The dome-shaped mountain has an elliptical base and a concave top, as well as other properties that indicate cryovolcanism. The authors applied models to determine the age of Ahuna Mons, finding it to have formed after the craters surrounding it, which suggests that it came into existence relatively recently. There is no evidence for compressional tectonism, nor for erosional features, the authors say; it appears that extrusion is a main driver behind the formation of Ahuna Mons. Although the exact material driving the cryovolcano cannot be determined without further data, the authors propose that chlorine salts, which have been previously detected in a different region of Ceres, could have been present with water ice below Ceres' surface and driven the chemical activity that formed Ahuna Mons. In a second study, Jean-Philippe Combe et al. A high resolution Dawn framing camera image of Ahuna describe the detection of water ice - exposed on the Mons. Image width is 30 km. Credit: NASA/JPL- surface of Ceres. The dwarf planet was known to Caltech/UCLA/MPS/DLR/IDA contain water ice, but water ice is also expected to be unstable on its surface, so scientists were unsure whether it could be detected there. They used the Visible and InfraRed (VIR) mapping Six studies published today in Science highlight spectrometer onboard the Dawn spacecraft to new and unexpected insights into Ceres, a dwarf analyze a highly reflective zone in a young crater planet and the largest object in the asteroid belt called Oxo, on five occasions during 2015. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Opening a New Chapter in the Martian Chronicles
California Institute of Technology Volume 2., No.• ~emlMr1"2 B•• ed on d.t. from the 1975 Viking ml ••lon , the Explore". Guide to MoIr • .... pon Arden Albee'. w a ll will be In for . ome updating once Ma ,. Ob.erve r be g in. It ••urv e v of the planet late ne xt vear. Albee ke ep. a replica of the .pacecraft In Caltech'. Office of Graduate Studle., w" .. e In addition to hi. role a. Ob.e rver project .clentl.t, he'. been dean . lnce1984. Opening a new chapter in the Martian Chronicles BV Heidi Aapaturlan Speaking this past August at a many Mars aficionados ever since the working in concert like an interplan "It's not cleat what sort of geologic NASA press conference called to herald Viking Lander's soil experimencs came etary one-man band, will monitor and dynamics might have produced this che upcoming launch of Mars Observer, up empty in 1975: has life ever map Mars with a sweep and precision dichotomy," says Albee, alchough he Cal tech Professor of Geology Arden evolved on Mars? Did the planet once that is expected to yield more informa suspects that the answer may start to Albee sounded ar rimes like a man who harbor a bacterial Atlantis that van tion abour the planer's composition, emerge once ic's determined whether had jusc been commissioned to write ished, along with its water, aeons ago? climate, geology, and evolutionary Mars, like Earth, has a magnetic field. the lyrics for the Marcian version of Although no one expects the Mars history than all previous miss ions co Currenc theory holds that a planet'S "America che Beauciful." "We know Observer, launched September 25 from Mars put together. -
Geologic Map of the Victoria Quadrangle (H02), Mercury
H01 - Borealis Geologic Map of the Victoria Quadrangle (H02), Mercury 60° Geologic Units Borea 65° Smooth plains material 1 1 2 3 4 1,5 sp H05 - Hokusai H04 - Raditladi H03 - Shakespeare H02 - Victoria Smooth and sparsely cratered planar surfaces confined to pools found within crater materials. Galluzzi V. , Guzzetta L. , Ferranti L. , Di Achille G. , Rothery D. A. , Palumbo P. 30° Apollonia Liguria Caduceata Aurora Smooth plains material–northern spn Smooth and sparsely cratered planar surfaces confined to the high-northern latitudes. 1 INAF, Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy; 22.5° Intermediate plains material 2 H10 - Derain H09 - Eminescu H08 - Tolstoj H07 - Beethoven H06 - Kuiper imp DiSTAR, Università degli Studi di Napoli "Federico II", Naples, Italy; 0° Pieria Solitudo Criophori Phoethontas Solitudo Lycaonis Tricrena Smooth undulating to planar surfaces, more densely cratered than the smooth plains. 3 INAF, Osservatorio Astronomico di Teramo, Teramo, Italy; -22.5° Intercrater plains material 4 72° 144° 216° 288° icp 2 Department of Physical Sciences, The Open University, Milton Keynes, UK; ° Rough or gently rolling, densely cratered surfaces, encompassing also distal crater materials. 70 60 H14 - Debussy H13 - Neruda H12 - Michelangelo H11 - Discovery ° 5 3 270° 300° 330° 0° 30° spn Dipartimento di Scienze e Tecnologie, Università degli Studi di Napoli "Parthenope", Naples, Italy. Cyllene Solitudo Persephones Solitudo Promethei Solitudo Hermae -30° Trismegisti -65° 90° 270° Crater Materials icp H15 - Bach Australia Crater material–well preserved cfs -60° c3 180° Fresh craters with a sharp rim, textured ejecta blanket and pristine or sparsely cratered floor. 2 1:3,000,000 ° c2 80° 350 Crater material–degraded c2 spn M c3 Degraded craters with a subdued rim and a moderately cratered smooth to hummocky floor. -
Ceramics from Wet-Processing of Martian Soil Simulant Using Slip Casting Or Additive Manufacturing for In-Situ Resource Utilization
DOI: 10.13009/EUCASS2019-769 Ceramics from wet-processing of Martian soil simulant using slip casting or Additive Manufacturing for in-situ resource utilization on Mars David Karl # *, Franz Kamutzki*, Andrea Zocca**, Pedro Lima**, Oliver Goerke*, Jens Guenster** and Aleksander Gurlo* * Fachgebiet Keramische Werkstoffe / Chair of Advanced Ceramic Materials, TU Berlin, Germany. ** Bundesanstalt für Materialforschung und –prüfung (BAM), Berlin, Germany. # Corresponding author. E-mail: [email protected] Abstract For future colonization of Planet Mars, the most realistic approach for the production of parts on site is in situ resource utilization (ISRU). In this study, we demonstrate the feasibility of this concept by producing objects of varying complexity exclusively using resources that can be found on the surface of Mars. The established production routes using slip casting and Additive Manufacturing via wet- processing of Mars simulant material are simple, robust and easily transferable even to the harsh conditions on Mars. After sintering our slip cast parts have mechanical properties comparable to commercially available porcelain, making them suitable for everyday use. 1. Introduction A promising concept for the exploration and subsequent colonization of Moon and Mars is in-situ resource utilization (ISRU) - collecting, processing and storing of native materials that are encountered during human or robotic space exploration [1]. Early colonization scenarios suggest the direct use of rock-covering loose granular surface media (including dust, soil and rubble) consisting of various oxide minerals called lunar and Mars regoliths. The chemical composition of lunar and Mars regolith makes the extraction of metals and ceramics conceivable. The availability of ceramic tools is an important prerequisite for melting regolith in blast furnaces and bloomeries for the production of base metals. -
Global Spectral Classification of Martian Low-Albedo Regions with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) Data A
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 112, E02004, doi:10.1029/2006JE002726, 2007 Global spectral classification of Martian low-albedo regions with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) data A. Deanne Rogers,1 Joshua L. Bandfield,2 and Philip R. Christensen2 Received 4 April 2006; revised 12 August 2006; accepted 13 September 2006; published 14 February 2007. [1] Martian low-albedo surfaces (defined here as surfaces with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) albedo values 0.15) were reexamined for regional variations in spectral response. Low-albedo regions exhibit spatially coherent variations in spectral character, which in this work are grouped into 11 representative spectral shapes. The use of these spectral shapes in modeling global surface emissivity results in refined distributions of previously determined global spectral unit types (Surface Types 1 and 2). Pure Type 2 surfaces are less extensive than previously thought, and are mostly confined to the northern lowlands. Regional-scale spectral variations are present within areas previously mapped as Surface Type 1 or as a mixture of the two surface types, suggesting variations in mineral abundance among basaltic units. For example, Syrtis Major, which was the Surface Type 1 type locality, is spectrally distinct from terrains that were also previously mapped as Type 1. A spectral difference also exists between southern and northern Acidalia Planitia, which may be due in part to a small amount of dust cover in southern Acidalia. Groups of these spectral shapes can be averaged to produce spectra that are similar to Surface Types 1 and 2, indicating that the originally derived surface types are representative of the average of all low-albedo regions. -
Program Schedule
Program Schedule AIAA Science and Technology Forum and Exposition 2015 January 05 - 09, 2015 The Program Report was last updated December 18, 2014 at 04:16 PM EST. To view the most recent meeting schedule online, visit https://aiaa-mst15.abstractcentral.com/planner.jsp Monday, January 05, 2015 Time Session or Event Info 8:00 AM-9:00 AM, Osceola Ballroom CD, PLNRY-01. Opening Keynote , Plenary, Forum 9:00 AM-12:30 PM, St. George 112, ISC-01. International Student Conference (Undergraduate Category), Technical Paper, 53rd AIAA Aerospace Sciences Meeting, Chair: Chris Tavares, The Boeing Company Martian RHOVER Feasibility Study J. Fuentes; R. Pankaja 9:00-9:30 AM Kaluarachchi Satellite Formation Control using Differential Drag S.R. Omar; J.M. 9:30-10:00 AM Wersinger Manufacturing of Triaxial Quasi-three-dimensional Composite 10:00-10:30 AM Materials G. Peterson; D. Liu The Design, Fabrication, and Evaluation of Millimeter Wave Lenses 10:30-11:00 AM for Beamed Energy Applications S.E. Sloan Colorimetric hydrogel-based microfluidic assay system to monitor 11:00-11:30 AM malnutrition in a microgravity environment J.K. Tsosie Significance of Constituent Chemical age on Solid Rocket Propellant 11:30-12:00 PM Regression Rates D.J. Dulin; G.S. Gibson 12:00-12:30 PM Aerodynamic Testing and Development of Sunswift eVe S. Ambrose 9:30 AM-12:30 PM, Miami 2, AA-01. Computational Aeroacoustics I, Technical Paper, 53rd AIAA Aerospace Sciences Meeting, Chair: Walter Eversman, Missouri University of Science and Technology A Computational Study of Flow Within Cavities with Complex 9:30-10:00 AM Geometric Features M.F. -
Water on the Moon, III. Volatiles & Activity
Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere). -
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