Non-Principal Axis Rotation (Tumbling) Asteroids
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Orbit Options for an Orion-Class Spacecraft Mission to a Near-Earth Object
Orbit Options for an Orion-Class Spacecraft Mission to a Near-Earth Object by Nathan C. Shupe B.A., Swarthmore College, 2005 A thesis submitted to the Faculty of the Graduate School of the University of Colorado in partial fulfillment of the requirements for the degree of Master of Science Department of Aerospace Engineering Sciences 2010 This thesis entitled: Orbit Options for an Orion-Class Spacecraft Mission to a Near-Earth Object written by Nathan C. Shupe has been approved for the Department of Aerospace Engineering Sciences Daniel Scheeres Prof. George Born Assoc. Prof. Hanspeter Schaub Date The final copy of this thesis has been examined by the signatories, and we find that both the content and the form meet acceptable presentation standards of scholarly work in the above mentioned discipline. iii Shupe, Nathan C. (M.S., Aerospace Engineering Sciences) Orbit Options for an Orion-Class Spacecraft Mission to a Near-Earth Object Thesis directed by Prof. Daniel Scheeres Based on the recommendations of the Augustine Commission, President Obama has pro- posed a vision for U.S. human spaceflight in the post-Shuttle era which includes a manned mission to a Near-Earth Object (NEO). A 2006-2007 study commissioned by the Constellation Program Advanced Projects Office investigated the feasibility of sending a crewed Orion spacecraft to a NEO using different combinations of elements from the latest launch system architecture at that time. The study found a number of suitable mission targets in the database of known NEOs, and pre- dicted that the number of candidate NEOs will continue to increase as more advanced observatories come online and execute more detailed surveys of the NEO population. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
CURRICULUM VITAE, ALAN W. HARRIS Personal: Born
CURRICULUM VITAE, ALAN W. HARRIS Personal: Born: August 3, 1944, Portland, OR Married: August 22, 1970, Rose Marie Children: W. Donald (b. 1974), David (b. 1976), Catherine (b 1981) Education: B.S. (1966) Caltech, Geophysics M.S. (1967) UCLA, Earth and Space Science PhD. (1975) UCLA, Earth and Space Science Dissertation: Dynamical Studies of Satellite Origin. Advisor: W.M. Kaula Employment: 1966-1967 Graduate Research Assistant, UCLA 1968-1970 Member of Tech. Staff, Space Division Rockwell International 1970-1971 Physics instructor, Santa Monica College 1970-1973 Physics Teacher, Immaculate Heart High School, Hollywood, CA 1973-1975 Graduate Research Assistant, UCLA 1974-1991 Member of Technical Staff, Jet Propulsion Laboratory 1991-1998 Senior Member of Technical Staff, Jet Propulsion Laboratory 1998-2002 Senior Research Scientist, Jet Propulsion Laboratory 2002-present Senior Research Scientist, Space Science Institute Appointments: 1976 Member of Faculty of NATO Advanced Study Institute on Origin of the Solar System, Newcastle upon Tyne 1977-1978 Guest Investigator, Hale Observatories 1978 Visiting Assoc. Prof. of Physics, University of Calif. at Santa Barbara 1978-1980 Executive Committee, Division on Dynamical Astronomy of AAS 1979 Visiting Assoc. Prof. of Earth and Space Science, UCLA 1980 Guest Investigator, Hale Observatories 1983-1984 Guest Investigator, Lowell Observatory 1983-1985 Lunar and Planetary Review Panel (NASA) 1983-1992 Supervisor, Earth and Planetary Physics Group, JPL 1984 Science W.G. for Voyager II Uranus/Neptune Encounters (JPL/NASA) 1984-present Advisor of students in Caltech Summer Undergraduate Research Fellowship Program 1984-1985 ESA/NASA Science Advisory Group for Primitive Bodies Missions 1985-1993 ESA/NASA Comet Nucleus Sample Return Science Definition Team (Deputy Chairman, U.S. -
Asteroid Touring Nanosatellite Fleet
Asteroid Touring Nanosatellite Fleet S Mihkel Pajusalu Postdoctoral fellow Massachusetts Institute of Technology (and Tartu Observatory) [email protected] + Pekka Janhunen, Andris Slavinskis, and the MAT collaboration Bio • 2010 MSc in Physics, University of Tartu, Estonia • 2010-2015 ESTCube-1 team, leader of Electrical Power Subsystem • 2014 PhD in Physics University of Tartu, Estonia • 2015 - 2019 Postdoc at MIT, Seager Group (astrobiology and instrumentation development for the MAT mission) Only 12 asteroids have been visited this far 1 Ceres Image Credit: NASA / 4 253 Mathilde 433 Eros JPL-Caltech / UCLA / Vesta NEAR /NASA NEAR Shoemaker MPS / DLR / IDA / Justin NASA/JPL/JHUAPL Cowart 951 Gaspra 243 Ida and 2867 Šteins 21 Lutetia Dactyl Galileo/NASA Rosetta ESA MPS ESA 2010 MPS for Galileo/NASA / JPL/USGS for OSIRIS Team OSIRIS Team MPS/UPD/LAM/IAA MPS/UPD/LAM/IAA/RSS D/INTA/UPM/DASP/IDA 9969 Braille 5535 Annefrank Deep Space 25143 Itokawa 4179 Toutatis Stardust/JPL/NASA 1/NASA/JPL/USGS Hayabusa/JAXA Chang’e/CNSA Multiple Asteroid Touring (MAT) mission See Slavinskis et al, “Nanospacecraft Fleet for Multi-asteroid Touring with Electric Solar Wind Sails”, IEEE Aerospace conference, 2018 Mission details • The reference mission contains 50 identical CubeSats • Estimated total cost <100 million USD • Each to visit 6 targets on average • 100 km – 1000 km flybys • Total of 300 visits during 3.2 years • Even if 50% are successful, number of visited asteroids would increase by a factor of 10 • First published concept from Finnish Meteorological -
4 from the Herschel-VVDS-CFHTLS-D1 Field
A&A 572, A90 (2014) Astronomy DOI: 10.1051/0004-6361/201323089 & c ESO 2014 Astrophysics Hidden starbursts and active galactic nuclei at 0 < z < 4 from the Herschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback B. C. Lemaux1,E.LeFloc’h2,O.LeFèvre1,O.Ilbert1, L. Tresse1,L.M.Lubin3, G. Zamorani4,R.R.Gal5, P. Ciliegi4, P. Cassata1,9,D.D.Kocevski6,7,E.J.McGrath7,S.Bardelli4, E. Zucca4, and G. K. Squires8 1 Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France e-mail: [email protected] 2 Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS – Université Paris Diderot, CE-Saclay, pt courrier 131, 91191 Gif-sur-Yvette, France 3 Department of Physics, University of California, Davis, 1 Shields Avenue, Davis, CA 95616, USA 4 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy 5 University of Hawai’i, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 6 Department of Physics and Astronomy, University of Kentucky, Lexington, KY 40506-0055, USA 7 Department of Physics and Astronomy, Colby College, Waterville, ME 04901, USA 8 Spitzer Science Center, California Institute of Technology, M/S 220-6, 1200 E. California Blvd., Pasadena, CA 91125, USA 9 Instituto de Fisica y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Gran Breta˜na 1111, Casilla 5030, Playa Ancha, Valparaíso, Chile Received 20 November 2013 / Accepted 17 September 2014 ABSTRACT We investigate of the properties of ∼2000 Herschel/SPIRE far-infrared-selected galaxies from 0 < z < 4intheCFHTLS-D1field. Using a combination of extensive spectroscopy from the VVDS and ORELSE surveys, deep multiwavelength imaging from CFHT, VLA, Spitzer, XMM-Newton,andHerschel, and well-calibrated spectral energy distribution fitting, Herschel-bright galaxies are com- pared to optically-selected galaxies at a variety of redshifts. -
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. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated. -
Near-Ir Spectroscopy and Possible Meteorite Analogs for Asteroid (253) Mathilde
Lunar and Planetary Science XXXVIII (2007) 2366.pdf NEAR-IR SPECTROSCOPY AND POSSIBLE METEORITE ANALOGS FOR ASTEROID (253) MATHILDE. Michael S. Kelley1, Michael J. Gaffey2 and Vishnu Reddy2, 1Department of Geology and Geography, Georgia Southern University, Statesboro, Georgia 30460-8149 [email protected] , 2Department of Space Studies, University of North Dakota, Grand Forks, ND 58202-9008 [email protected] and [email protected] . Introduction: Main-belt asteroid (253) Mathilde Bokkevelt & Murray (CM2). The the ~0.9 µm feature was discovered November 12, 1885 by J. Palisa at Vi- is evident in all of these spectra. enna. It was probably named in honor of Mathilde, née Worms, wife of the astronomer Moritz Loewy (1833-1907), vice-director of the Paris Observatory [1]. Prior to the 1980s Mathilde received little atten- tion aside from astrometric measurements. The asteroid was included in spectrophotometric surveys in the mid-late 1980s [2-4], and in the IRAS survey [5]. These studies provided albedo and diame- ter estimates, and sufficient information to classify Mathilde as a C-type asteroid. Mathilde became the subject of intense interest in the 1990s when it was announced that the asteroid would be the target of a spacecraft flyby. Various studies provided rotation rate, size estimates, and addi- tional spectrophotometric data [6,7]. Based on these newer data, and existing analyses of carbonaceous chondrites, Mathilde was interpreted as having a sur- face dominated by either strongly heated carbonaceous Figure 1 – Normalized reflectance spectrum of chondrite materials (to an extent not seen in meteorite Mathilde (SpeX & SMASS data) compared to the CI1 collections), or a shock-darkened ordinary chondritic chondrite Orgueil [10] (red line). -
Appendix 1 1311 Discoverers in Alphabetical Order
Appendix 1 1311 Discoverers in Alphabetical Order Abe, H. 28 (8) 1993-1999 Bernstein, G. 1 1998 Abe, M. 1 (1) 1994 Bettelheim, E. 1 (1) 2000 Abraham, M. 3 (3) 1999 Bickel, W. 443 1995-2010 Aikman, G. C. L. 4 1994-1998 Biggs, J. 1 2001 Akiyama, M. 16 (10) 1989-1999 Bigourdan, G. 1 1894 Albitskij, V. A. 10 1923-1925 Billings, G. W. 6 1999 Aldering, G. 4 1982 Binzel, R. P. 3 1987-1990 Alikoski, H. 13 1938-1953 Birkle, K. 8 (8) 1989-1993 Allen, E. J. 1 2004 Birtwhistle, P. 56 2003-2009 Allen, L. 2 2004 Blasco, M. 5 (1) 1996-2000 Alu, J. 24 (13) 1987-1993 Block, A. 1 2000 Amburgey, L. L. 2 1997-2000 Boattini, A. 237 (224) 1977-2006 Andrews, A. D. 1 1965 Boehnhardt, H. 1 (1) 1993 Antal, M. 17 1971-1988 Boeker, A. 1 (1) 2002 Antolini, P. 4 (3) 1994-1996 Boeuf, M. 12 1998-2000 Antonini, P. 35 1997-1999 Boffin, H. M. J. 10 (2) 1999-2001 Aoki, M. 2 1996-1997 Bohrmann, A. 9 1936-1938 Apitzsch, R. 43 2004-2009 Boles, T. 1 2002 Arai, M. 45 (45) 1988-1991 Bonomi, R. 1 (1) 1995 Araki, H. 2 (2) 1994 Borgman, D. 1 (1) 2004 Arend, S. 51 1929-1961 B¨orngen, F. 535 (231) 1961-1995 Armstrong, C. 1 (1) 1997 Borrelly, A. 19 1866-1894 Armstrong, M. 2 (1) 1997-1998 Bourban, G. 1 (1) 2005 Asami, A. 7 1997-1999 Bourgeois, P. 1 1929 Asher, D. -
Non-Principal Axis Rotation (Tumbling) Asteroids
NON-PRINCIPAL AXIS ROTATION (TUMBLING) ASTEROIDS Asteroid PAR Per1 Amp1 Per2 Amp2 Reference 244 Sita T0 129.51 0.82 0 129.51 0.82 Brinsfield, 09 253 Mathilde T 417.7 0.50 –3 417.7 0.45 250. Mottola, 95 –3 418. 0.5 250. Pravec, 05 288 Glauke T 1170. 0.9 –1 1200. 0.9 Harris, 99 0 Pravec, 14 –2 1170. 0.37 740. Pilcher, 15 299 Thora T0 274. 0.39 0 274. 0.39 Pilcher, 14 408 Fama T0 202.1 0.58 0 202.1 0.58 Stephens, 08 470 Kilia T0 290. 0.26 0 290. 0.26 Stephens, 09 0 Stephens, 09 571 Dulcinea T 126.3 0.50 –2 126.3 0.50 Stephens, 11 630 Euphemia T0 350. 0.45 0 350. 0.45 Warner, 11 707 Ste¨ına T0 414. 1.00 0 Pravec, 14 823 Sisigambis T0 146. 0.7 0 Pravec, 14 824 Anastasia T– 250. 1.20 +2 250. 1.20 Stephens, 10 +2 Pravec, 14 846 Lipperta T0 1641. 0.30 0 1641. 0.30 Buchheim, 11 887 Alinda T0 73.97 0.35 0 Pravec, 14 912 Maritima T0 1332. 0.18 0 Pravec, 14 950 Ahrensa T0 202. 0.40 0 Pravec, 14 989 Schwassmannia T0 107.85 0.39 0 107.85 0.35 Benishek, 14 0 120.3 0.39 Stephens, 14 1042 Amazone T0 540. 0.25 0 Pravec, 14 1183 Jutta T0 212.5 0.10 0 212.5 0.10 Stephens, 11 1235 Schorria T0 1265. -
Cloudy with a Chance of Near-Earth Asteroids
Cloudy with a chance of near-Earth asteroids KU LEUVEN - UGENT MASTER OF SPACE STUDIES 2018-2019 CORNEEL BOGAERT Space Sciences and Exploration Professor: C. Waelkens Table of contents Introduction ................................................................................................................................. 1 1. Asteroids .................................................................................................................................. 2 1.1 Near-Earth asteroids ..................................................................................................................... 3 2. Potentially hazardous asteroids ................................................................................................ 4 2.1 Remote sensing from Earth ........................................................................................................... 5 2.2 Missions in space ........................................................................................................................... 6 3. Exploration missions to NEAs .................................................................................................... 8 3.1 Asteroid flybys ............................................................................................................................... 8 3.2 NEAR Shoemaker ........................................................................................................................... 9 3.3 Hayabusa (MUSES-C) & Hayabusa2 ............................................................................................