2008 Medals & Awards G.K. Gilbert Award
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MARS ODYSSEY at a GLANCE High-Gain Antenna
years 20 ar ound th Mars Odyssey’s future remains unknown, but a lack of advocacy might indicate its end is near. BY NOLA TAYLOR REDD hen NASA’s While Odyssey is nevertheless Odyssey managing to still carry out its job in spacecraft space, it’s struggling in the political Wblasted off in arena. President Trump’s 2021 bud- 2001, Mars was get request, released in February considered a dry, barren world. 2020, most clearly threatened mis- But over the past two decades, this sions like SOFIA, a telescope that quiet powerhouse of an orbiter has flies on a plane. However, the revealed a wealth of information danger to Odyssey was more subtle: about the Red Planet. During its Trump’s 2021 budget slashes first year around Mars, Odyssey Odyssey’s funding from just under found the first direct evidence $12 million to around $1 million. of subsurface water on This would effectively pull the plug the planet. The orbiter on a working spacecraft, whose pri- also currently holds the mary costs are human maintenance record for the longest and guidance. continuous observa- But “Odyssey is remarkably tions of martian healthy,” says Phil Christensen, the weather, which is principal investigator for Odyssey’s an ongoing study Thermal Emission Imaging System with important (THEMIS) and a geologist at implications for Arizona State University. “It’s just ABOVE: The 2001 Mars future human this crazy workhorse spacecraft that Odyssey space- habitation rarely goes into safe mode.” craft launched April 7, 2001, aboard a of Mars. Boeing Delta II rocket, Twenty years of Two decades of science starting a seven-month wear and tear have undoubtedly Odyssey arrived at Mars on journey to the Red Planet. -
Placing World War I in the History of Mathematics David Aubin, Catherine Goldstein
Placing World War I in the History of Mathematics David Aubin, Catherine Goldstein To cite this version: David Aubin, Catherine Goldstein. Placing World War I in the History of Mathematics. 2013. hal- 00830121v1 HAL Id: hal-00830121 https://hal.sorbonne-universite.fr/hal-00830121v1 Preprint submitted on 4 Jun 2013 (v1), last revised 8 Jul 2014 (v2) HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Placing World War I in the History of Mathematics David Aubin and Catherine Goldstein Abstract. In the historical literature, opposite conclusions were drawn about the impact of the First World War on mathematics. In this chapter, the case is made that the war was an important event for the history of mathematics. We show that although mathematicians' experience of the war was extremely varied, its impact was decisive on the life of a great number of them. We present an overview of some uses of mathematics in war and of the development of mathematics during the war. We conclude by arguing that the war also was a crucial factor in the institutional modernization of mathematics. Les vrais adversaires, dans la guerre d'aujourd'hui, ce sont les professeurs de math´ematiques`aleur table, les physiciens et les chimistes dans leur laboratoire. -
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. -
The Tricky Business of Identifying Rocks on Mars
PSRD: Using TES to interpret the composition of the Martian surface http://www.psrd.hawaii.edu/May02/MarsTES.html posted May 22, 2002 The Tricky Business of Identifying Rocks on Mars --- A new analysis of thermal emission spectra suggests a new interpretation for the composition of the Martian surface. Written by G. Jeffrey Taylor Hawai'i Institute of Geophysics and Planetology The Mars Global Surveyor mission carries a remote-sensing gizmo called the Thermal Emission Spectrometer (TES). TES detects heat waves flowing from the surface of the Red Planet. The TES team, led by Phil Christensen (Arizona State University), identified two large regions on Mars that have distinctive spectral properties. Using mathematical mixing calculations based on the thermal emission spectra of numerous materials, the TES team reported in papers led by Josh Bandfield and Victoria Hamilton that the two regions had mineral abundances similar to basalt (Surface Type 1) and andesite (Surface Type 2), two common volcanic rock types on Earth. Andesite has more silicon than does basalt, giving rise to a distinctive mineralogy. Scientists had mixed reactions to the possibility of andesite on Mars, greeting the news with fascination, consternation, or skepticism. One question raised is how uniquely the spectra of Surface Type 2 matches andesite. Michael Wyatt and Harry Y. McSween (University of Tennessee) have taken another look at the TES spectra by using a larger collection of aqueous alteration (weathering) products in the spectral mixing calculations. They show that weathered basalt also matches the spectral properties of Surface Type 2. Wyatt and McSween also note that Type 2 regions are generally confined to a large, low region that is the site of a purported Martian ocean that sloshed around billions of years ago. -
Discrete Element Modelling of Pit Crater Formation on Mars
geosciences Article Discrete Element Modelling of Pit Crater Formation on Mars Stuart Hardy 1,2 1 ICREA (Institució Catalana de Recerca i Estudis Avançats), Passeig Lluís Companys 23, 08010 Barcelona, Spain; [email protected]; Tel.: +34-934-02-13-76 2 Departament de Dinàmica de la Terra i de l’Oceà, Facultat de Ciències de la Terra, Universitat de Barcelona, C/Martí i Franqués s/n, 08028 Barcelona, Spain Abstract: Pit craters are now recognised as being an important part of the surface morphology and structure of many planetary bodies, and are particularly remarkable on Mars. They are thought to arise from the drainage or collapse of a relatively weak surficial material into an open (or widening) void in a much stronger material below. These craters have a very distinctive expression, often presenting funnel-, cone-, or bowl-shaped geometries. Analogue models of pit crater formation produce pits that typically have steep, nearly conical cross sections, but only show the surface expression of their initiation and evolution. Numerical modelling studies of pit crater formation are limited and have produced some interesting, but nonetheless puzzling, results. Presented here is a high-resolution, 2D discrete element model of weak cover (regolith) collapse into either a static or a widening underlying void. Frictional and frictional-cohesive discrete elements are used to represent a range of probable cover rheologies. Under Martian gravitational conditions, frictional-cohesive and frictional materials both produce cone- and bowl-shaped pit craters. For a given cover thickness, the specific crater shape depends on the amount of underlying void space created for drainage. -
Mineralogy of the Martian Surface
EA42CH14-Ehlmann ARI 30 April 2014 7:21 Mineralogy of the Martian Surface Bethany L. Ehlmann1,2 and Christopher S. Edwards1 1Division of Geological & Planetary Sciences, California Institute of Technology, Pasadena, California 91125; email: [email protected], [email protected] 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109 Annu. Rev. Earth Planet. Sci. 2014. 42:291–315 Keywords First published online as a Review in Advance on Mars, composition, mineralogy, infrared spectroscopy, igneous processes, February 21, 2014 aqueous alteration The Annual Review of Earth and Planetary Sciences is online at earth.annualreviews.org Abstract This article’s doi: The past fifteen years of orbital infrared spectroscopy and in situ exploration 10.1146/annurev-earth-060313-055024 have led to a new understanding of the composition and history of Mars. Copyright c 2014 by Annual Reviews. Globally, Mars has a basaltic upper crust with regionally variable quanti- by California Institute of Technology on 06/09/14. For personal use only. All rights reserved ties of plagioclase, pyroxene, and olivine associated with distinctive terrains. Enrichments in olivine (>20%) are found around the largest basins and Annu. Rev. Earth Planet. Sci. 2014.42:291-315. Downloaded from www.annualreviews.org within late Noachian–early Hesperian lavas. Alkali volcanics are also locally present, pointing to regional differences in igneous processes. Many ma- terials from ancient Mars bear the mineralogic fingerprints of interaction with water. Clay minerals, found in exposures of Noachian crust across the globe, preserve widespread evidence for early weathering, hydrothermal, and diagenetic aqueous environments. Noachian and Hesperian sediments include paleolake deposits with clays, carbonates, sulfates, and chlorides that are more localized in extent. -
Long-Term Historical and Projected Herbivore Population Dynamics in Ngorongoro Crater, Tanzania
PLOS ONE RESEARCH ARTICLE Long-term historical and projected herbivore population dynamics in Ngorongoro crater, Tanzania 1³ 2³ 2 3 Patricia D. Moehlman , Joseph O. OgutuID *, Hans-Peter Piepho , Victor A. Runyoro , Michael B. Coughenour4, Randall B. Boone5 1 IUCN/SSC Equid Specialist Group, Arusha, Arusha, Tanzania, 2 Institute for Crop Science-340, University of Hohenheim, Stuttgart, Germany, 3 Environmental Reliance Consultants Limited, Arusha, Tanzania, 4 Department of Ecosystem Science and Sustainability, Colorado State University, Fort Collins, Colorado, United States of America, 5 Natural Resource Ecology Laboratory, Colorado State University, Fort Collins, a1111111111 Colorado, United States of America a1111111111 a1111111111 ³ PDM and JOO are joint first authors on this work. a1111111111 * [email protected] a1111111111 Abstract The Ngorongoro Crater is an intact caldera with an area of approximately 310 km2 located OPEN ACCESS within the Ngorongoro Conservation Area (NCA) in northern Tanzania. It is known for the Citation: Moehlman PD, Ogutu JO, Piepho H-P, abundance and diversity of its wildlife and is a UNESCO World Heritage Site and an Interna- Runyoro VA, Coughenour MB, Boone RB (2020) tional Biosphere Reserve. Long term records (1963±2012) on herbivore populations, vege- Long-term historical and projected herbivore population dynamics in Ngorongoro crater, tation and rainfall made it possible to analyze historic and project future herbivore population Tanzania. PLoS ONE 15(3): e0212530. https://doi. dynamics. NCA was established as a multiple use area in 1959. In 1974 there was a pertur- org/10.1371/journal.pone.0212530 bation in that resident Maasai and their livestock were removed from the Ngorongoro Crater. -
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 -
The Very Forward CASTOR Calorimeter of the CMS Experiment
EUROPEAN ORGANIZATION FOR NUCLEAR RESEARCH (CERN) CERN-EP-2020-180 2021/02/11 CMS-PRF-18-002 The very forward CASTOR calorimeter of the CMS experiment The CMS Collaboration* Abstract The physics motivation, detector design, triggers, calibration, alignment, simulation, and overall performance of the very forward CASTOR calorimeter of the CMS exper- iment are reviewed. The CASTOR Cherenkov sampling calorimeter is located very close to the LHC beam line, at a radial distance of about 1 cm from the beam pipe, and at 14.4 m from the CMS interaction point, covering the pseudorapidity range of −6.6 < h < −5.2. It was designed to withstand high ambient radiation and strong magnetic fields. The performance of the detector in measurements of forward energy density, jets, and processes characterized by rapidity gaps, is reviewed using data collected in proton and nuclear collisions at the LHC. ”Published in the Journal of Instrumentation as doi:10.1088/1748-0221/16/02/P02010.” arXiv:2011.01185v2 [physics.ins-det] 10 Feb 2021 © 2021 CERN for the benefit of the CMS Collaboration. CC-BY-4.0 license *See Appendix A for the list of collaboration members Contents 1 Contents 1 Introduction . .1 2 Physics motivation . .3 2.1 Forward physics in proton-proton collisions . .3 2.2 Ultrahigh-energy cosmic ray air showers . .5 2.3 Proton-nucleus and nucleus-nucleus collisions . .5 3 Detector design . .6 4 Triggers and operation . .9 5 Event reconstruction and calibration . 12 5.1 Noise and baseline . 13 5.2 Gain correction factors . 15 5.3 Channel-by-channel intercalibration . -
The OSIRIS-Rex Thermal Emission Spectrometer (OTES) Instrument
Manuscript The OSIRIS-REx Thermal Emission Spectrometer (OTES) Instrument P.R. Christensen1, V.E. Hamilton2, G.L. Mehall1, D. Pelham1, W. O’Donnell1, S. Anwar1, H. Bowles1, S. Chase1, J. Fahlgren1, Z. Farkas1, T. Fisher1, O. James3, I. Kubik1, I. Lazbin4, M. Miner1, M. Rassas1, L. Schulze1, K. Shamordola1, T. Tourville1, G. West4, R. Woodward1, D. Lauretta5 1School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA Phone: 480-965-7105 ([email protected]) 2Southwest Research Institute, Boulder, CO, USA 3Goddard Space Flight Center, Greenbelt, MD, USA 4Moog Broad Reach, Tempe, AZ; currently at AZ Space Technologies, Gilbert, AZ, USA 5University of Arizona, Tucson, AZ, USA Abstract The OSIRIS-REx Thermal Emission Spectrometer (OTES) will provide remote measurements of mineralogy and thermophysical properties of Bennu to map its surface, help select the OSIRIS-REx sampling site, and investigate the Yarkovsky effect. OTES is a Fourier Transform spectrometer covering the spectral range 5.71– 100 µm (1750–100 cm–1) with a spectral sample interval of 8.66 cm–1 and a 6.5-mrad field of view. The OTES telescope is a 15.2-cm diameter Cassegrain telescope that feeds a flat-plate Michelson moving mirror mounted on a linear voice-coil motor assembly. A single uncooled deuterated L-alanine doped triglycine sulfate (DLATGS) pyroelectric detector is used to sample the interferogram every two seconds. Redundant ~0.855 µm laser diodes are used in a metrology interferometer to provide precise moving mirror control and IR sampling at 772 Hz. The beamsplitter is a 38-mm diameter, 1-mm thick chemical vapor deposited diamond with an antireflection microstructure to minimize surface reflection. -
The Rationale for a Long-Lived Geophysical
THE RATIONALE FOR A LONG-LIVED GEOPHYSICAL NETWORK MISSION TO MARS Submitted to The Mars Panel, NRC Decadal Survey for the Planetary Sciences Division, SMD, NASA Phil Christensen, Chair; Wendy Calvin, Vice Chair Written by Bruce Banerdt JPL Robert Grimm SwRI Franck Montmessin Scot Rafkin SwRI Tilman Spohn DLR Matthias Grott DLR Service Aeronomie Peter Read Oxford Ulli Christensen MPS Bob Haberle NASA-Ames Yosio Nakamura Gerald Schubert UCLA Veronique Dehant ROB Martin Knapmeyer DLR U Texas (ret.) Sue Smrekar JPL Linda Elkins-Tanton MIT Philippe Lognonné IPGP Roger Phillips SwRI Mike Wilson JPL Endorsed by Oded Aharonson Caltech François Forget Kurt Klaus Boeing Thomas Ruedas Carnegie Don Albert CRREL CNRS-LMD Jörg Knollenberg DLR Chris Russell UCLA Carlton Allen NASA-JSC Matt Fouch ASU Naoki Kobayashi JAXA David Sandwell Scripps Robert Anderson JPL Brenda Franklin JPL Ulrich Koehler DLR Nicholas Schmerr Carnegie Scott Anderson SwRI Herbert Frey GSFC Carlos Lange U Alberta Nicole Schmitz DLR Jeff Andrews-Hanna Jeannine Gagnepain- Gary Latham DOE (ret.) Richard Schultz U Nevada Colo. School of Mines Beyneix IPGP Mark Leese Open U Mindi Searls U Colorado Jafar Arkani-Hamed Rafael Garcia Frank Lemoine GSFC Karsten Seiferlin U Bern McGill U Obs. Midi-Pyrenees Robert Lillis UC Berkeley Nikolai Shapiro IPGP Gabriele Arnold U Münster Jim Garvin GSFC John Longhi Charles Shearer UNM Sami Asmar JPL Rebecca Ghent U Toronto Lamont-Doherty Brian Shiro NOAA Lisa Baldwin DLR Domenico Giardini ETH Paul Lundgren JPL Mark Simons Caltech Don Banfield Cornell Lori Glaze GSFC Mioara Mandea GFZ Norman Sleep Stanford Amy Barr SwRI Matthew Golombek JPL Michael Manga John C. -
Onboard Detection of Thermal Anomalies for Europa Clipper
EPSC Abstracts Vol. 12, EPSC2018-528-2, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Onboard Detection of Thermal Anomalies for Europa Clipper Gary Doran (1), Ashley G. Davies (1), Kiri L. Wagstaff (1), Saadat Anwar (2), Diana L. Blaney (1), Steve Chien (1), Phil Christensen (2), and Serina Diniega (1). (1) Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, (2) Arizona State University, Tempe, AZ, USA ([email protected]) 1. Introduction targets, without human intervention [4]. A previous study determined that the THEMIS instrument in Mars The Europa Clipper mission seeks to assess the habit- orbit could reliably detect thermal anomalies, aerosols, ability of Jupiter’s moon Europa [6, 1]. Europa Clip- and ice features of interest [3]. per’s payload comprises nine instruments, including Europa observations of high interest include those the Europa Thermal Emission Imaging System (E- containing thermal and spectral anomalies that could THEMIS) for detecting thermal anomalies (e.g., hot signal the presence of hot spots, plumes, or deposits of spots) and the Mapping Imaging Spectrometer for Eu- organic materials at the surface. Any thermal anoma- ropa (MISE) for assessing composition. E-THEMIS lies detected in E-THEMIS data can also potentially can detect melting ice and other surface anomalies inform prioritization of coincident MISE data during from 40,000 km above the surface. MISE covers the closer approach in the same flyby. range 0.8–5.0 µm and can distinguish between water ice phases, organics, salts, etc. [2]. 2. THEMIS Anomaly Detection Europa Clipper will conduct 45 flybys of Europa.