Daniel J. Scheeres, Phd. Degrees Professional Positions
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Dirk Brouwer
NATIONAL ACADEMY OF SCIENCES D I R K B R O U W ER 1902—1966 A Biographical Memoir by G . M . C LEMENCE Any opinions expressed in this memoir are those of the author(s) and do not necessarily reflect the views of the National Academy of Sciences. Biographical Memoir COPYRIGHT 1970 NATIONAL ACADEMY OF SCIENCES WASHINGTON D.C. DIRK BROUWER September 1, 1902-January 31, 1966 BY G. M. CLEMENCE IRK BROUWER, who contributed more to dynamical astron- D omy than any other astronomer of his time, died on January 31, 1966, after a week in hospital; his death was occa- sioned by an acute disorder of the heart. He is survived by his widow and an only son, James. Brouwer was born in Rotterdam, the Netherlands, on September 1, 1902, the son of a civil service employee. As a stu- dent in the University of Leiden he studied mathematics and astronomy, coming under the influence of Willem de Sitter, who in his own day was the dean of that branch of astronomy in which Brouwer was to do most of his work. Receiving the Ph.D. degree in 1927 under de Sitter, Brouwer came to the United States as a fellow of the International Education Board, spending a year at the University of California in Berkeley and at Yale University, where he was to remain the rest of his life. His initial appointment at Yale was in 1928 as research as- sistant to Ernest W. Brown, who was then the greatest living authority on the motion of the moon. -
Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa
dsc_cover (Converted)-1 8/6/02 10:33 AM Page 1 Deep Space Chronicle Deep Space Chronicle: A Chronology ofDeep Space and Planetary Probes, 1958–2000 |Asif A.Siddiqi National Aeronautics and Space Administration NASA SP-2002-4524 A Chronology of Deep Space and Planetary Probes 1958–2000 Asif A. Siddiqi NASA SP-2002-4524 Monographs in Aerospace History Number 24 dsc_cover (Converted)-1 8/6/02 10:33 AM Page 2 Cover photo: A montage of planetary images taken by Mariner 10, the Mars Global Surveyor Orbiter, Voyager 1, and Voyager 2, all managed by the Jet Propulsion Laboratory in Pasadena, California. Included (from top to bottom) are images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus, and Neptune. The inner planets (Mercury, Venus, Earth and its Moon, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. NASA SP-2002-4524 Deep Space Chronicle A Chronology of Deep Space and Planetary Probes 1958–2000 ASIF A. SIDDIQI Monographs in Aerospace History Number 24 June 2002 National Aeronautics and Space Administration Office of External Relations NASA History Office Washington, DC 20546-0001 Library of Congress Cataloging-in-Publication Data Siddiqi, Asif A., 1966 Deep space chronicle: a chronology of deep space and planetary probes, 1958-2000 / by Asif A. Siddiqi. p.cm. – (Monographs in aerospace history; no. 24) (NASA SP; 2002-4524) Includes bibliographical references and index. 1. Space flight—History—20th century. I. Title. II. Series. III. NASA SP; 4524 TL 790.S53 2002 629.4’1’0904—dc21 2001044012 Table of Contents Foreword by Roger D. -
Near Earth Asteroid Rendezvous: Mission Summary 351
Cheng: Near Earth Asteroid Rendezvous: Mission Summary 351 Near Earth Asteroid Rendezvous: Mission Summary Andrew F. Cheng The Johns Hopkins Applied Physics Laboratory On February 14, 2000, the Near Earth Asteroid Rendezvous spacecraft (NEAR Shoemaker) began the first orbital study of an asteroid, the near-Earth object 433 Eros. Almost a year later, on February 12, 2001, NEAR Shoemaker completed its mission by landing on the asteroid and acquiring data from its surface. NEAR Shoemaker’s intensive study has found an average density of 2.67 ± 0.03, almost uniform within the asteroid. Based upon solar fluorescence X-ray spectra obtained from orbit, the abundance of major rock-forming elements at Eros may be consistent with that of ordinary chondrite meteorites except for a depletion in S. Such a composition would be consistent with spatially resolved, visible and near-infrared (NIR) spectra of the surface. Gamma-ray spectra from the surface show Fe to be depleted from chondritic values, but not K. Eros is not a highly differentiated body, but some degree of partial melting or differentiation cannot be ruled out. No evidence has been found for compositional heterogeneity or an intrinsic magnetic field. The surface is covered by a regolith estimated at tens of meters thick, formed by successive impacts. Some areas have lesser surface age and were apparently more recently dis- turbed or covered by regolith. A small center of mass offset from the center of figure suggests regionally nonuniform regolith thickness or internal density variation. Blocks have a nonuniform distribution consistent with emplacement of ejecta from the youngest large crater. -
Asteroids Upclose
Asteroids UpClose Quick Views of Big Advances Asteroids Up Close The importance of spacecraft missions in the quest to understand asteroids is highlighted in a recent review paper by Thomas Burbine (Mount Holyoke College, Massachusettes). Burbine discusses achievements in understanding the chemistries and mineralogies of asteroids since the launch of NASA's NEAR-Shoemaker robotic spacecraft in 1996, the first mission dedicated to asteroid exploration. As two new robotic asteroid-sample-return missions are underway (NASA's OSIRIS-REx and JAXA's Hayabusa2), Burbine's review paper and a review by Derek Sears earlier this year (see the January 2016 PSRD CosmoSparks: Comprehending Asteroids) provide timely recaps of why asteroids are so important to our understanding of the building Simulated cratering and topography are overlaid on blocks of our Solar System. radar imagery of asteroid Bennu — one of the next asteroids to be visited up close by NASA's OSIRIS- Burbine reviews these mission highlights: REx mission. Click image for more information from University of Arizona News. NEAR-Shoemaker (NASA mission) flew by (253) Mathilde, a C-complex asteroid. It orbited and landed on (433) Eros, an S-type asteroid, and used an X-ray spectrometer to determine elemental ratios, which were consistent with a body that did not melt globally. Most likely meteorite matches for Eros are surface-altered ordinary chondrites or primitive achondrites. For more see PSRD article: The Composition of Asteroid 433 Eros. Hayabusa (JAXA mission) was a touch-and-go mission to (25143) Itokawa, an S-complex asteroid. It carried a multiband imager, near-infrared spectrometer, laser altimeter, LIDAR, X-ray spectrometer, and a sample capsule. -
Final Report Asteroid Impact Monitoring
Final Report Asteroid Impact Monitoring Environmental and Instrumentation Requirements A component of the Asteroid Impact & Deflection Assessment (AIDA) Mission By the AIM Advisory Team Dr. Patrick MICHEL (Univ. Nice, CNRS, OCA), Team Leader Dr. Jens Biele (DLR) Dr. Marco Delbo (Univ. Nice, CNRS, OCA) Dr. Martin Jutzi (Univ. Bern) Pr. Guy Libourel (Univ. Nice, CNRS, OCA) Dr. Naomi Murdoch Dr. Stephen R. Schwartz (Univ. Nice, CNRS, OCA) Dr. Stephan Ulamec (DLR) Dr. Jean-Baptiste Vincent (MPS) April 12th, 2014 Introduction In this report, we describe the knowledge gain resulting from the implementation of either the European Space Agency’s Asteroid Impact Monitoring (AIM) as a stand- alone mission or AIM with its second component, the Double Asteroid Redirection Test (DART) mission under study by the Johns Hopkins Applied Physics Laboratory with support from members of NASA centers including Goddard Space Flight Center, Johnson Space Center, and the Jet Propulsion Laboratory. We then present our analysis of the required measurements addressing the goals of the AIM mission to the binary Near-Earth Asteroid (NEA) Didymos, and for two specified payloads. The first payload is a mini thermal infrared camera (called TP1) for short and medium range characterisation. The second payload is an active seismic experiment (called TP2). We then present the environmental parameters for the AIM mission. AIM is a rendezvous mission that focuses on the monitoring aspects i.e., the capability to determine in-situ the key properties of the secondary of a binary asteroid. DART consists primarily of an artificial projectile aims to demonstrate asteroid deflection. In the framework of the full AIDA concept, AIM will also give access to the detailed conditions of the DART impact and its outcome, allowing for the first time to get a complete picture of such an event, a better interpretation of the deflection measurement and a possibility to compare with numerical modeling predictions. -
Frank Schlesinger 1871-1943
NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA BIOGRAPHICAL MEMOIRS VOLUME XXIV THIRD MEMOIR BIOGRAPHICAL MEMOIR OF FRANK SCHLESINGER 1871-1943 BY DIRK BROUWER PRESENTED TO THE ACADEMY AT THE ANNUAL MEETING, 1945 FRANK SCHLESINGER 1871-1943 BY DIRK BROUWER Frank Schlesinger was born in New York City on May n, 1871. His father, William Joseph Schlesinger (1836-1880), and his mother, Mary Wagner Schlesinger (1832-1892), both natives of the German province of Silesia, had emigrated to the United States. In Silesia they had lived in neighboring vil- lages, but they did not know each other until they met in New York, in 1855, at the home of Mary's cousin. They were mar- ried in 1857 and had seven children, all of whom grew to maturity. Frank was the youngest and, after 1939, the last survivor. His father's death, in 1880, although it brought hardships to the family, was not permitted to interfere with Frank's educa- tion. He attended public school in New York City, and eventually entered the College of the City of New York, receiv- ing the degree of Bachelor of Science in 1890. His aptitude for mathematical science, already evident in grammar school, be- came more marked in the higher stages of his education when he began to show a preference for applied mathematics. Upon completing his undergraduate work it was not possible for him to continue with graduate studies. He had to support himself, and his health at that time made it desirable for him to engage in outdoor activities. -
NL#153 July/August
AAAS Publication for the members N of the Americanewsletter Astronomical Society July/August 2010, Issue 153 CONTENTS President's Column Debra Meloy Elmegreen, [email protected] 2 th From the Moon over Miami, palm trees, and a riverwalk set the perfect scene for our 216 meeting, a typically intimate summer gathering with about 800 attendees. Kudos and thanks to Kevin and Executive Office his Marvel-ous staff for another smooth and well-executed gathering. It was all the more special because of meeting jointly with the Solar Physics Division, which happens every three years. It is nice when the smaller divisions are able to overlap with the general meeting, to foster more interactions among astronomers who work in a variety of fields. Dramatic results from new 3 missions such as Herschel, Hinode and SDO, WISE, CoRot, Cassini-Huygens observations of Journals Update Titan, CMB observations from the South Pole, progress on ALMA, and solar tales from SPD Hale prize winner Marcia Neugebauer and Harvey prize winner Brian Welsch were among the many exciting presentations. 4 Three newly funded opportunities were announced: the Doxsey Award for thesis-presenting Council Actions graduate students to travel to the AAS, the Lancelot Berkeley Prize for meritorious recently published research to be presented at the AAS, and the Kavli Award to a distinguished plenary AAS speaker, as discussed elsewhere in this Newsletter. 5 I was thinking about what makes AAS meetings special. We gather for the science, of course; the general meetings provide opportunities to get a firsthand update on key advances, which help Secretary's Corner inform not only our research but also our teaching. -
The Landing of the NEAR-Shoemaker Spacecraft on Asteroid 433 Eros
letters to nature ................................................................. images were buffered in real-time and then played back while the next The landing of the NEAR-Shoemaker set was being acquired. All images were shuttered using an exposure of 15 ms to limit smear. Here we summarize the major insights spacecraft on asteroid 433 Eros about the surface of Eros obtained from the images. More detailed analyses of speci®c observations are provided in accompanying 5 4 J. Veverka*, B. Farquhar², M. Robinson³, P. Thomas*, S. Murchie², contributions describing ponded deposits and ejecta blocks . A. Harch*, P. G. Antreasian§, S. R. Chesley§, J. K. Miller§, The selection of the landing site was dictated by several practical W. M. Owen Jr§, B. G. Williams§, D. Yeomans§, D. Dunham², G. Heyler², considerations that are summarized in the legend to Fig. 1. One aim M. Holdridge², R. L. Nelson², K. E. Whittenburg², J. C. Ray², B. Carcich*, was to land the NEAR spacecraft in a region where details of surface A. Cheng², C. Chapmank, J. F. Bell III*, M. Bell*, B. Bussey³, B. Clark*, modi®cation by ejecta and downslope movement of regolith could D. Domingue², M. J. Gaffey¶, E. Hawkins², N. Izenberg², J. Joseph*, be studied. We hoped to land in the vicinity of one of the enigmatic R. Kirk#, P. LuceyI, M. Malin**, L. McFadden²², W. J. Merlinek, `ponds' discovered during the 28 October 2000 low-altitude ¯yby6 C. Peterson*, L. Prockter², J. Warren² & D. Wellnitz²² and viewed at even better resolution (0.5 m) in late January 2001. The location of the landing site, within the 9-km depression * Space Sciences Building, Cornell University, Ithaca, New York 14853, USA Himeros, is shown in Fig. -
An Innovative Solution to NASA's NEO Impact Threat Mitigation Grand
Final Technical Report of a NIAC Phase 2 Study December 9, 2014 NASA Grant and Cooperative Agreement Number: NNX12AQ60G NIAC Phase 2 Study Period: 09/10/2012 – 09/09/2014 An Innovative Solution to NASA’s NEO Impact Threat Mitigation Grand Challenge and Flight Validation Mission Architecture Development PI: Dr. Bong Wie, Vance Coffman Endowed Chair Professor Asteroid Deflection Research Center Department of Aerospace Engineering Iowa State University, Ames, IA 50011 email: [email protected] (515) 294-3124 Co-I: Brent Barbee, Flight Dynamics Engineer Navigation and Mission Design Branch (Code 595) NASA Goddard Space Flight Center Greenbelt, MD 20771 email: [email protected] (301) 286-1837 Graduate Research Assistants: Alan Pitz (M.S. 2012), Brian Kaplinger (Ph.D. 2013), Matt Hawkins (Ph.D. 2013), Tim Winkler (M.S. 2013), Pavithra Premaratne (M.S. 2014), Sam Wagner (Ph.D. 2014), George Vardaxis, Joshua Lyzhoft, and Ben Zimmerman NIAC Program Executive: Dr. John (Jay) Falker NIAC Program Manager: Jason Derleth NIAC Senior Science Advisor: Dr. Ronald Turner NIAC Strategic Partnerships Manager: Katherine Reilly Contents 1 Hypervelocity Asteroid Intercept Vehicle (HAIV) Mission Concept 2 1.1 Introduction ...................................... 2 1.2 Overview of the HAIV Mission Concept ....................... 6 1.3 Enabling Space Technologies for the HAIV Mission . 12 1.3.1 Two-Body HAIV Configuration Design Tradeoffs . 12 1.3.2 Terminal Guidance Sensors/Algorithms . 13 1.3.3 Thermal Protection and Shield Issues . 14 1.3.4 Nuclear Fuzing Mechanisms ......................... 15 2 Planetary Defense Flight Validation (PDFV) Mission Design 17 2.1 The Need for a PDFV Mission ............................ 17 2.2 Preliminary PDFV Mission Design by the MDL of NASA GSFC . -
Dawn Mission Reveals Dwarf Planet Else in the Solar System
Fossil Planet With lowlands, highlands, weird white spots, and even a pyramid, the largest object in the asteroid belt is unlike anything Dawn mission reveals dwarf planet else in the solar system. by Eric Betz IN THE BEGINNING, with a mass equivalent to just 4 percent of that contained in Earth’s Moon. What was OUR SOLAR SYSTEM left is what we still see today. One-third of that mass is held by a single WAS A VIOLENT PLACE. world, Ceres. At 590 miles (950 kilometers) NASA’s Dawn mission Radiation from neighboring massive across, it’s our solar system’s largest asteroid captured Ceres from stars bombarded our small part of a large and the only dwarf planet this side of Pluto. Ceres 8,400 miles (13,600 kilometers) away in molecular cloud — a many light-years-wide It’s also a relic of our violent origins. May as it spiraled body of gas and dust resembling the Eagle This icy body is the current focus of into ever-lower Nebula’s “Pillars of Creation” — as the NASA’s Dawn mission — a small spacecraft orbits. ALL IMAGES: NASA/ JPL-CALTECH/UCLA/MPS/DLR/IDA, whole expanse coalesced like a figure skater that’s powered its way across the inner solar EXCEPT WHERE NOTED pulling her limbs in tight for a spin. system since 2007 using unconventional Some 99.8 percent of the mass drew to ion propulsion. The engine allowed Dawn the center, forming our Sun. And out of the to become the first mission to ever orbit firmament 4.6 billion years ago, tiny bits of two extraterrestrial bodies. -
Near Earth Asteroid Thermal Modeling
42nd Lunar and Planetary Science Conference (2011) 2583.pdf Near Earth Asteroid Thermal Modeling [NEATM] and Thermophysical Modeling of 10 low albedo NEAs using Infrared Spectrograph (IRS) on NASA’s Spitzer Space Telescope R.Dave1([email protected]), J.P. Emery1([email protected]), 1Univ. Tennessee. Introduction: Near-Earth Asteroids (NEAs- the peak in thermal emission. These data enable more 0.983AU<q<1.3AU) are fragments of remnant accurate and detailed modeling of the surface primordial bodies dating since the formation of Solar temperature distributions. System. Information about the albedo and size Observations: Spitzer observed the ten asteroids in distribution of the NEAs is an essential prerequisite for this study between June 2004 and April 2006. Thermal exploring their physical nature, thermal properties, spectra from 5.2 to 38 µm were measured with the mineralogy, taxonomy and for developing reliable NEA Infrared Spectrograph (IRS), which collects data in four population models [1]. In support of the ExploreNEOs different modules: campaign of the Warm Spitzer program, the current Low-resolution, short-wavelength - 5.2 - 14 microns, project is a study of a sample of NEAs using the Infrared Low-resolution, long-wavelength - 14 - 38 microns, Spectrograph (IRS) on NASA’s Spitzer Space Telescope High-resolution, short-wavelength - 10 - 19.5 microns, [Programs 88 and 91- Extinct Comets and Low- albedo High-resolution, long-wavelength - 19 - 37 microns. Asteroids]. The 5.2-38 m thermal emission µ The spectra analyzed here use only the low-spectral spectra[R~60- 130] are fitted with models of the thermal resolution modules (R=λ/Δλ~64 to 128). -
– Near-Earth Asteroid Mission Concept Study –
ASTEX – Near-Earth Asteroid Mission Concept Study – A. Nathues1, H. Boehnhardt1 , A. W. Harris2, W. Goetz1, C. Jentsch3, Z. Kachri4, S. Schaeff5, N. Schmitz2, F. Weischede6, and A. Wiegand5 1 MPI for Solar System Research, 37191 Katlenburg-Lindau, Germany 2 DLR, Institute for Planetary Research, 12489 Berlin, Germany 3 Astrium GmbH, 88039 Friedrichshafen, Germany 4 LSE Space AG, 82234 Oberpfaffenhofen, Germany 5 Astos Solutions, 78089 Unterkirnach, Germany 6 DLR GSOC, 82234 Weßling, Germany ASTEX Marco Polo Symposium, Paris 18.5.09, A. Nathues - 1 Primary Objectives of the ASTEX Study Identification of the required technologies for an in-situ mission to two near-Earth asteroids. ¾ Selection of realistic mission scenarios ¾ Definition of the strawman payload ¾ Analysis of the requirements and options for the spacecraft bus, the propulsion system, the lander system, and the launcher ASTEX ¾ Definition of the requirements for the mission’s operational ground segment Marco Polo Symposium, Paris 18.5.09, A. Nathues - 2 ASTEX Primary Mission Goals • The mission scenario foresees to visit two NEAs which have different mineralogical compositions: one “primitive'‘ object and one fragment of a differentiated asteroid. • The higher level goal is the provision of information and constraints on the formation and evolution history of our planetary system. • The immediate mission goals are the determination of: – Inner structure of the targets – Physical parameters (size, shape, mass, density, rotation period and spin vector orientation) – Geology, mineralogy, and chemistry ASTEX – Physical surface properties (thermal conductivity, roughness, strength) – Origin and collisional history of asteroids – Link between NEAs and meteorites Marco Polo Symposium, Paris 18.5.09, A.