Nj. R*Tt N R | Ji I MI I
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Thickness of the Martian Crust: Improved Constraints from Geoid-To-Topography Ratios Mark A
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 109, E01009, doi:10.1029/2003JE002153, 2004 Thickness of the Martian crust: Improved constraints from geoid-to-topography ratios Mark A. Wieczorek De´partement de Ge´ophysique Spatiale et Plane´taire, Institut de Physique du Globe de Paris, Saint-Maur, France Maria T. Zuber Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA Received 10 July 2003; revised 1 September 2003; accepted 24 November 2003; published 24 January 2004. [1] The average crustal thickness of the southern highlands of Mars was investigated by calculating geoid-to-topography ratios (GTRs) and interpreting these in terms of an Airy compensation model appropriate for a spherical planet. We show that (1) if GTRs were interpreted in terms of a Cartesian model, the recovered crustal thickness would be underestimated by a few tens of kilometers, and (2) the global geoid and topography signals associated with the loading and flexure of the Tharsis province must be removed before undertaking such a spatial analysis. Assuming a conservative range of crustal densities (2700–3100 kg mÀ3), we constrain the average thickness of the Martian crust to lie between 33 and 81 km (or 57 ± 24 km). When combined with complementary estimates based on crustal thickness modeling, gravity/topography admittance modeling, viscous relaxation considerations, and geochemical mass balance modeling, we find that a crustal thickness between 38 and 62 km (or 50 ± 12 km) is consistent with all studies. Isotopic investigations based on Hf-W and Sm-Nd systematics suggest that Mars underwent a major silicate differentiation event early in its evolution (within the first 30 Ma) that gave rise to an ‘‘enriched’’ crust that has since remained isotopically isolated from the ‘‘depleted’’ mantle. -
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, -
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). -
In Pdf Format
lós 1877 Mik 88 ge N 18 e N i h 80° 80° 80° ll T 80° re ly a o ndae ma p k Pl m os U has ia n anum Boreu bal e C h o A al m re u c K e o re S O a B Bo l y m p i a U n d Planum Es co e ria a l H y n d s p e U 60° e 60° 60° r b o r e a e 60° l l o C MARS · Korolev a i PHOTOMAP d n a c S Lomono a sov i T a t n M 1:320 000 000 i t V s a Per V s n a s l i l epe a s l i t i t a s B o r e a R u 1 cm = 320 km lkin t i t a s B o r e a a A a A l v s l i F e c b a P u o ss i North a s North s Fo d V s a a F s i e i c a a t ssa l vi o l eo Fo i p l ko R e e r e a o an u s a p t il b s em Stokes M ic s T M T P l Kunowski U 40° on a a 40° 40° a n T 40° e n i O Va a t i a LY VI 19 ll ic KI 76 es a As N M curi N G– ra ras- s Planum Acidalia Colles ier 2 + te . -
Sir George Biddell Airy (1801 – 1892)
Sir George Biddell Airy (1801 – 1892) From Wikipedia, the free encyclopedia, http://en.wikipedia.org/wiki/George_Biddell_Airy Sir George Biddell Airy PRS KCB was an English mathematician and astronomer, Astronomer Royal from 1835 to 1881. His many achievements include work on planetary orbits, measuring the mean density of the Earth, a method of solution of two-dimensional problems in solid mechanics and, in his role as Astronomer Royal, establishing Greenwich as the location of the prime meridian. His reputation has been tarnished by allegations that, through his inaction, Britain lost the opportunity of priority in the discovery of Neptune. Biography: Airy was born at Alnwick, one of a long line of Airys who traced their descent back to a family of the same name residing at Kentmere, in Westmorland, in the 14th century. The branch to which he belonged, having suffered in the English Civil War, moved to Lincolnshire and became farmers. Airy was educated first at elementary schools in Hereford, and afterwards at Colchester Royal Grammar School. An introverted child, Airy gained popularity with his schoolmates through his great skill in the construction of peashooters. From the age of 13, Airy stayed frequently with his uncle, Arthur Biddell at Playford, Suffolk. Biddell introduced Airy to his friend Thomas Clarkson, the slave trade abolitionist who lived at Playford Hall. Clarkson had an MA in mathematics from Cambridge, and examined Airy in classics and then subsequently arranged for him to be examined by a Fellow from Trinity College, Cambridge on his knowledge of mathematics. As a result he entered Trinity in 1819, as a sizar, meaning that he paid a reduced fee but essentially worked as a servant to make good the fee reduction. -
Ebook < Impact Craters on Mars # Download
7QJ1F2HIVR # Impact craters on Mars « Doc Impact craters on Mars By - Reference Series Books LLC Mrz 2012, 2012. Taschenbuch. Book Condition: Neu. 254x192x10 mm. This item is printed on demand - Print on Demand Neuware - Source: Wikipedia. Pages: 50. Chapters: List of craters on Mars: A-L, List of craters on Mars: M-Z, Ross Crater, Hellas Planitia, Victoria, Endurance, Eberswalde, Eagle, Endeavour, Gusev, Mariner, Hale, Tooting, Zunil, Yuty, Miyamoto, Holden, Oudemans, Lyot, Becquerel, Aram Chaos, Nicholson, Columbus, Henry, Erebus, Schiaparelli, Jezero, Bonneville, Gale, Rampart crater, Ptolemaeus, Nereus, Zumba, Huygens, Moreux, Galle, Antoniadi, Vostok, Wislicenus, Penticton, Russell, Tikhonravov, Newton, Dinorwic, Airy-0, Mojave, Virrat, Vernal, Koga, Secchi, Pedestal crater, Beagle, List of catenae on Mars, Santa Maria, Denning, Caxias, Sripur, Llanesco, Tugaske, Heimdal, Nhill, Beer, Brashear Crater, Cassini, Mädler, Terby, Vishniac, Asimov, Emma Dean, Iazu, Lomonosov, Fram, Lowell, Ritchey, Dawes, Atlantis basin, Bouguer Crater, Hutton, Reuyl, Porter, Molesworth, Cerulli, Heinlein, Lockyer, Kepler, Kunowsky, Milankovic, Korolev, Canso, Herschel, Escalante, Proctor, Davies, Boeddicker, Flaugergues, Persbo, Crivitz, Saheki, Crommlin, Sibu, Bernard, Gold, Kinkora, Trouvelot, Orson Welles, Dromore, Philips, Tractus Catena, Lod, Bok, Stokes, Pickering, Eddie, Curie, Bonestell, Hartwig, Schaeberle, Bond, Pettit, Fesenkov, Púnsk, Dejnev, Maunder, Mohawk, Green, Tycho Brahe, Arandas, Pangboche, Arago, Semeykin, Pasteur, Rabe, Sagan, Thira, Gilbert, Arkhangelsky, Burroughs, Kaiser, Spallanzani, Galdakao, Baltisk, Bacolor, Timbuktu,... READ ONLINE [ 7.66 MB ] Reviews If you need to adding benefit, a must buy book. Better then never, though i am quite late in start reading this one. I discovered this publication from my i and dad advised this pdf to find out. -- Mrs. Glenda Rodriguez A brand new e-book with a new viewpoint. -
Surface Properties of Asteroids from Mid-Infrared Observations and Thermophysical Modeling
Dissertation zur Erlangung des akademischen Grades Doktor der Naturwissenschaften (doctor rerum naturalium) Surface Properties of Asteroids from Mid-Infrared Observations and Thermophysical Modeling Dipl.-Phys. Michael M¨uller 2007 Eingereicht und verteidigt am Fachbereich Geowissenschaften der Freien Universit¨atBerlin. Angefertigt am Institut f¨ur Planetenforschung des Deutschen Zentrums f¨urLuft- und Raumfahrt e.V. (DLR) in Berlin-Adlershof. arXiv:1208.3993v1 [astro-ph.EP] 20 Aug 2012 Gutachter Prof. Dr. Ralf Jaumann (Freie Universit¨atBerlin, DLR Berlin) Prof. Dr. Tilman Spohn (Westf¨alische Wilhems-Universit¨atM¨unster,DLR Berlin) Tag der Disputation 6. Juli 2007 In loving memory of Felix M¨uller(1948{2005). Wish you were here. Abstract The subject of this work is the physical characterization of asteroids, with an emphasis on the thermal inertia of near-Earth asteroids (NEAs). Thermal inertia governs the Yarkovsky effect, a non-gravitational force which significantly alters the orbits of asteroids up to ∼ 20 km in diameter. Yarkovsky-induced drift is important in the assessment of the impact hazard which NEAs pose to Earth. Yet, very little has previously been known about the thermal inertia of small asteroids including NEAs. Observational and theoretical work is reported. The thermal emission of aster- oids has been observed in the mid-infrared (5{35 µm) wavelength range using the Spitzer Space Telescope and the 3.0 m NASA Infrared Telescope Facility, IRTF; techniques have been established to perform IRTF observations remotely from Berlin. A detailed thermophysical model (TPM) has been developed and exten- sively tested; this is the first detailed TPM shown to be applicable to NEA data. -
UCGE Reports Number 20191
UCGE Reports Number 20191 Department of Geomatics Engineering Simulation and Evaluation of the Performance of the Proposed Mars Network Constellation for Positioning, Orbit Improvement, and Establishment of a Spatial Reference Frame for Mars (URL: http://www.geomatics.ucalgary.ca/links/GradTheses.html) by Kyle O’Keefe April 2004 THE UNIVERSITY OF CALGARY Simulation and Evaluation of the Performance of the Proposed Mars Network Constellation for Positioning, Orbit Improvement, and Establishment of a Spatial Reference Frame for Mars by Kyle O’Keefe A THESIS SUBMITTED TO THE FACULTY OF GRADUATE STUDIES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY DEPARTMENT OF GEOMATICS ENGINEERING CALGARY, ALBERTA April, 2004 c Kyle O’Keefe 2004 Preface This is an unaltered version of the author’s Doctoral of Philosophy thesis. The thesis was accepted by the Faculty of Graduate Studies in April, 2004. The faculty supervisor for this work was Dr. G´erard Lachapelle. The co-supervisor was Dr. Susan Skone. Other members of the examining committee were Dr. M. Elizabeth Cannon, Dr. Patrick Wu, Dr. Wayne Cannon. ii Abstract In 1999, the NASA Jet Propulsion Lab presented a proposal for a six satellite nav- igation and communication network for Mars called the Mars Network. This thesis investigates the performance of the Mars Network both theoretically, using figures of merit commonly applied to satellite navigation systems on Earth, and in the position domain using simulated observations. The Mars Network is evaluated in terms of availability, accuracy, and reliability as a function of position and time by simulating network geometry for users distributed across the planet. -
Appendix 3 Särkinen Et Al
Appendix 3 Särkinen et al. – Old World Black Nightshades Appendix 3. Specimens examined Solanum alpinum INDONESIA. Sin. loc, Without Collector s.n. (L); Bali: bei der Quelle Jaritie auf Weg zum Gunung Ajaung, 2 Jun 1912, Arens 19 (L); Kleine Soenda Eilanden, Bali, Z. helling G. Agoeng, 6 Apr 1936, van Steenis 7839 (K); Java: Central Java, Blumbang, Mt. Lawu, Central Java, 26 Nov 1982, Afriastini 475 (A); West Java, MtMalabar, Oct 1861, Anderson 367 (CAL); West Java, MtMalabar, Oct 1861, Anderson 369 (CAL); West Java, G[unung] Guntar., 1861, Anderson 432 (CAL); East Java, Ardjoeno, tjemarabosch boven Lalidjiwo, 17 Oct 1915, Arens s.n. (L); East Java, 12 Oct 1915, Arens 48 (L); East Java, Pasoeroean, G[unung] Tengge, boven Tosari, 4 Jun 1913, Backer 8380 (L); East Java, Te Pasoeroean, Ngadisari, Jan 1925, Backer 36563 (A); East Java, Pasoeroean, S. Tengge, boven Tosari, Backer 36564 (L); Central Java, Soerkarta, Top van de Lawoe, 16 Jul 1936, Brinkman 754 (NY); Sitiebondo, G[unung] Raneg [Raoeng] via Brembeinri, 15 May 1932, Clason-Laarman, E.H.H. 157 (L); East Java, south east Java (CAL sheet has locality Malawar, Praesingar, 6000ft[?] but very hard to read), 18 Mar 1880, Forbes 1019 (BM, CAL); Central Java, Central Java, Slamet Mountain, 17 Mar 2004, Hoover et al. 113 (A); Central Java, MtPrahu, Horsfield s.n. (BM); Central Java, Surakarta, Horsfield s.n. (BM); Central Java, MtPrahu, Horsfield s.n. (BM); Central Java, Blambangan & Mt. Prahu, Horsfield s.n. (BM); sin. loc, Horsfield s.n. (K); sin. loc, Horsfield 5 (K); Sello, purchased 1859, Horsfield 5 (K); Sin. -
13. Martian Cratering and Implications for the Chronostratigraphy
13. Martian Cratering and Implications for the Chronostratigraphy The record of large impact basins on differ- ent planetary bodies allows us to compare the characteristics of the heavy bombardment pe- riod and the end of planetary formation. Both the cratering record itself and the age distri- bution of the impact basins represent the pe- riod of highest impactor flux, decaying rapidly within the first half billion years of our solar system. In order to test the plausibility of the Martian chronology model (see Chapter 5), the ages of the large Martian impact basins, using the derived Martian production function, were determined and compared to lunar basin ages. For the Moon, the large basins were produced no later than about 3.8 to 3.9 Ga ago and a similar situation should exist for Mars, follow- ing the marker horizon idea (Wetherill, 1975). This idea is based on the assumption that solar system bodies have undergone a similar evo- lution since planetary formation. In the cra- Figure 13.1.: The crater size frequency distribu- tering record on any solid surface body, which tion measured for one of the oldest regions on Mars: has representative large old surface units, this Noachis Terra (map nomenclature: unit Npl1). first period of heavy bombardment is present in the general crater size–frequency distribution as well as the large basin record itself. According to our investigation, the oldest surface areas on than the visible highland surface, where crater Mars, roughly the Martian southern highlands, count ages are based on craters clearly recog- e. g. Noachis Terra, were formed between 4.0 nized by their morphology. -
Bulk Mineralogy of Lunar Crater Central Peaks Via Thermal Infrared Spectra from the Diviner Lunar Radiometer - a Study of the Moon’S Crustal Composition at Depth
Bulk mineralogy of Lunar crater central peaks via thermal infrared spectra from the Diviner Lunar Radiometer - A study of the Moon’s crustal composition at depth Eugenie Song A thesis submitted in partial fulfillment of the requirements for the degree of Master of Sciences University of Washington 2012 Committee: Joshua Bandfield Alan Gillespie Bruce Nelson Program Authorized to Offer Degree: Earth and Space Sciences 1 Table of Contents List of Figures ............................................................................................................................................... 3 List of Tables ................................................................................................................................................ 3 Abstract ......................................................................................................................................................... 4 1 Introduction .......................................................................................................................................... 5 1.1 Formation of the Lunar Crust ................................................................................................... 5 1.2 Crater Morphology ................................................................................................................... 7 1.3 Spectral Features of Rock-Forming Silicates in the Lunar Environment ................................ 8 1.4 Compositional Studies of Lunar Crater Central Peaks ........................................................... -
Recent Aeolian Dune Change on Mars ⁎ M.C
Available online at www.sciencedirect.com Geomorphology 94 (2008) 247–255 www.elsevier.com/locate/geomorph Recent aeolian dune change on Mars ⁎ M.C. Bourke a,b, , K.S. Edgett c, B.A. Cantor c a Planetary Science Institute, Tucson, AZ 85719, USA b School of Geography and the Environment, University of Oxford, Oxford, OX1 3QY, UK c Malin Space Science Systems, PO Box 910148, San Diego, CA 92191-0148, USA Received 26 January 2007; received in revised form 24 May 2007; accepted 24 May 2007 Available online 8 June 2007 Abstract Previous comparisons of Martian aeolian dunes in satellite images have not detected any change in dune form or position. Here, we show dome dunes in the north polar region that shrank and then disappeared over a period of 3.04 Mars years (5.7 Earth years), while larger, neighboring dunes showed no erosion or movement. The removal of sand from these dunes indicates that not only is the threshold wind speed for saltation exceeded under present conditions on Mars, but that any sand that is available for transport is likely to be moved. Dunes that show no evidence of change could be crusted, indurated, or subject to infrequent episodes of movement. © 2007 Elsevier B.V. All rights reserved. Keywords: Mars; Aeolian; Dune; Sediment transport 1. Introduction dust is raised by wind somewhere on the planet nearly every Martian day (Cantor, 2003; Cantor et al., 2006; Aeolian bedforms are found at all latitudes on Mars Cantor, 2007). As sand is mobilized at a lower threshold (Thomas, 1982). Their presence requires that sand-sized friction speed than dust (Iverson and White, 1982), and material has been transported by saltation (Cutts and the impact of saltating grains will raise dust at threshold Smith, 1973).