Orbit and Bulk Density of the OSIRIS-Rex Target Asteroid (101955) Bennu
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The Orbit of the Minor Planet (7) Iris
ACTA ASTRONOMICA Vol. 43 (1993) pp. 177±181 The Orbit of the Minor Planet (7) Iris by I. Wøodarczyk Astronomical Observatory of the ChorzÂow Planetarium, 41-501 Chorz Âow 1, P.O. box 10, Poland. Received December 17, 1992, ®nal version received in May 1993 ABSTRACT 30 precise positions from the ChorzÂow Observatory and 15 observations from 3 others obser- vatories of (7) Iris made in 1991 are used to determine the orbit of this minor planet. The orbit was determined using once the SAO Catalogue and once the PPM Catalogue. The latter orbit ®ts better to all the observations. Key words: Minor planets ± Astrometry 1. TheChorzow Observations The photographic observations of (7) Iris were made with the photographic camera 200 1000 mm attached to the refractor 300 4500 mm. The geographical 0 00 h m s = = h = coordinates of this refractor are 1 15 58.52, 50 17 31. 8, 328 m. The ORWO plates ZU-21 16 16 cm were measured with the coordinate measur- ing instrument Ascorecord E-2. For the reduction of these plates the Turner method with the complete second- order polynomial was used. On every plate 10 to 14 reference stars were chosen (together 50 stars were considered). The coordinates and the proper motions of all stars were taken once from the SAO Catalogue for the epoch 19500 and once from the PPM Catalogue for the epoch 2000.0. Our positions of (7) Iris obtained with the SAO Catalogue are given in Table 1. There are observations made in 1991 during the opposition of (7) Iris in Nov. -
OSIRIS-Rex, Returning the Asteroid Sample
OSIRIS-REx, Returning the Asteroid Sample Thomas Ajluni Timothy Linn William Willcockson ASRC Federal Space & Defense Lockheed Martin Space Systems Lockheed Martin Space Systems 7000 Muirkirk Meadows Drive Company, P.O. Box 179 Company, P.O. Box 179 Suite 100, Beltsville, MD 20705 Denver, CO 80201 Denver, CO 80201 301.286.1831 303-977-0659 303-977-5094 [email protected] [email protected] [email protected] David Everett Ronald Mink Joshua Wood NASA Goddard Space Flight NASA Goddard Space Flight Lockheed Martin Space Systems Center, 8800 Greenbelt Road Center, 8800 Greenbelt Road Company, P.O. Box 179 Greenbelt, MD 20771 Greenbelt, MD 20771 Denver, CO 80201 301.286.1596 301.286.3524 303-977-3199 [email protected] [email protected] [email protected] Abstract—This paper addresses the technical aspects of the sample return system for the upcoming Origins, Spectral x attitude control Interpretation, Resource Identification, and Security-Regolith x propulsion Explorer (OSIRIS-REx) asteroid sample return mission. The x power overall mission design and current implementation are presented as an overview to establish a context for the x thermal control technical description of the reentry and landing segment of the x telecommunications mission. x command and data handling x structural support to ensure successful rendezvous The prime objective of the OSIRIS-REx mission is to sample a with Bennu primitive, carbonaceous asteroid and to return that sample to Earth in pristine condition for detailed laboratory analysis. x characterization of Bennu’s properties Targeting the near-Earth asteroid Bennu, the mission launches x delivery of the sampler to the surface, and return of in September 2016 with an Earth reentry date of September the spacecraft to the vicinity of the Earth 24, 2023. -
Cohesive Forces Prevent the Rotational Breakup of Rubble-Pile Asteroid (29075) 1950 DA
Open Research Online The Open University’s repository of research publications and other research outputs Cohesive forces prevent the rotational breakup of rubble-pile asteroid (29075) 1950 DA Journal Item How to cite: Rozitis, Ben; MacLennan, Eric and Emery, Joshua P. (2014). Cohesive forces prevent the rotational breakup of rubble-pile asteroid (29075) 1950 DA. Nature, 512(7513), article no. 13632. For guidance on citations see FAQs. c 2014 Macmillan Publishers Limited https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Accepted Manuscript Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1038/nature13632 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Cohesive forces preventing rotational breakup of rubble pile asteroid (29075) 1950 DA Ben Rozitis1, Eric MacLennan1 & Joshua P. Emery1 1Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, US ([email protected]) Space missions1 and ground-based observations2 have shown that some asteroids are loose collections of rubble rather than solid bodies. The physical behavior of such ‘rubble pile’ asteroids has been traditionally described using only gravitational and frictional forces within a granular material3. Cohesive forces in the form of small van der Waals forces between constituent grains have been recently predicted to be important for small rubble piles (10- kilometer-sized or smaller), and can potentially explain fast rotation rates in the small asteroid population4-6. -
Radar Imaging of Asteroid 7 Iris
Icarus 207 (2010) 285–294 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Radar imaging of Asteroid 7 Iris S.J. Ostro a,1, C. Magri b,*, L.A.M. Benner a, J.D. Giorgini a, M.C. Nolan c, A.A. Hine c, M.W. Busch d, J.L. Margot e a Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA b University of Maine at Farmington, 173 High Street – Preble Hall, Farmington, ME 04938, USA c Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA d Division of Geological and Planetary Sciences, California Institute of Technology, MC 150-21, Pasadena, CA 91125, USA e Department of Earth and Space Sciences, University of California, Los Angeles, 595 Charles Young Drive East, Box 951567, Los Angeles, CA 90095, USA article info abstract Article history: Arecibo radar images of Iris obtained in November 2006 reveal a topographically complex object whose Received 26 June 2009 gross shape is approximately ellipsoidal with equatorial dimensions within 15% of 253 Â 228 km. The Revised 10 October 2009 radar view of Iris was restricted to high southern latitudes, precluding reliable estimation of Iris’ entire Accepted 7 November 2009 3D shape, but permitting accurate reconstruction of southern hemisphere topography. The most promi- Available online 24 November 2009 nent features, three roughly 50-km-diameter concavities almost equally spaced in longitude around the south pole, are probably impact craters. In terms of shape regularity and fractional relief, Iris represents a Keywords: plausible transition between 50-km-diameter asteroids with extremely irregular overall shapes and Asteroids very large concavities, and very much larger asteroids (Ceres and Vesta) with very regular, nearly convex Radar observations shapes and generally lacking monumental concavities. -
Jjmonl 1503.Pmd
alactic Observer GJohn J. McCarthy Observatory Volume 8, No. 3 March 2015 Gaslight District the birth of a star is hailed in the brightness of its surrounding dust and gas . But why the patch of darkness in the center? Find out more inside, page 19 The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky It is through their efforts that the McCarthy Observatory Technical Support has established itself as a significant educational and Bob Lambert recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Allison Jim Johnstone Steve Barone Carly KleinStern Colin Campbell Bob Lambert Dennis Cartolano Roger Moore Route Mike Chiarella Parker Moreland, PhD Jeff Chodak Allan Ostergren Bill Cloutier Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Randy Finden Gene Schilling John Gebauer Katie Shusdock Elaine Green Jon Wallace Paul Tina Hartzell Woodell Tom Heydenburg Amy Ziffer In This Issue "OUT THE WINDOW ON YOUR LEFT" ............................... 4 SUNRISE AND SUNSET ...................................................... 15 RUPES RECTA ................................................................ 5 JUPITER AND ITS MOONS ................................................. 15 THE TWINS EXPERIMENT ................................................ -
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. -
The Minor Planet Bulletin and How the Situation Has Gone from One Mt Tarana Observatory of Trying to Fill Pages to One of Fitting Everything In
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 2, A.D. 2006 APRIL-JUNE 29. PHOTOMETRY OF ASTEROIDS 133 CYRENE, adjusted up or down to line up with the V-band data). The near- 454 MATHESIS, 477 ITALIA, AND 2264 SABRINA perfect overlay of V- and R-band data show no evidence of color change as the asteroid rotates. This result replicates the lightcurve Robert K. Buchheim period reported by Harris et al. (1984), and matches the period and Altimira Observatory lightcurve shape reported by Behrend (2005) at his website. 18 Altimira, Coto de Caza, CA 92679 USA [email protected] (Received: 4 November Revised: 21 November) Photometric studies of asteroids 133 Cyrene, 454 Mathesis, 477 Italia and 2264 Sabrina are reported. The lightcurve period for Cyrene of 12.707±0.015 h (with amplitude 0.22 mag) confirms prior studies. The lightcurve period of 8.37784±0.00003 h (amplitude 0.32 mag) for Mathesis differs from previous studies. For Italia, color indices (B-V)=0.87±0.07, (V-R)=0.48±0.05, and phase curve parameters H=10.4, G=0.15 have been determined. For Sabrina, this study provides the first reported lightcurve period 43.41±0.02 h, with 0.30 mag amplitude. Altimira Observatory, located in southern California, is equipped with a 0.28-m Schmidt-Cassegrain telescope (Celestron NexStar- 454 Mathesis. DiMartino et al. (1994) reported a rotation period of 11 operating at F/6.3), and CCD imager (ST-8XE NABG, with 7.075 h with amplitude 0.28 mag for this asteroid, based on two Johnson-Cousins filters). -
Stardust Sample Return
National Aeronautics and Space Administration Stardust Sample Return Press Kit January 2006 www.nasa.gov Contacts Merrilee Fellows Policy/Program Management (818) 393-0754 NASA Headquarters, Washington DC Agle Stardust Mission (818) 393-9011 Jet Propulsion Laboratory, Pasadena, Calif. Vince Stricherz Science Investigation (206) 543-2580 University of Washington, Seattle, Wash. Contents General Release ............................................................................................................... 3 Media Services Information ……………………….................…………….................……. 5 Quick Facts …………………………………………..................………....…........…....….. 6 Mission Overview …………………………………….................……….....……............…… 7 Recovery Timeline ................................................................................................ 18 Spacecraft ………………………………………………..................…..……...........……… 20 Science Objectives …………………………………..................……………...…..........….. 28 Why Stardust?..................…………………………..................………….....………............... 31 Other Comet Missions .......................................................................................... 33 NASA's Discovery Program .................................................................................. 36 Program/Project Management …………………………........................…..…..………...... 40 1 2 GENERAL RELEASE: NASA PREPARES FOR RETURN OF INTERSTELLAR CARGO NASA’s Stardust mission is nearing Earth after a 2.88 billion mile round-trip journey -
Constraining Mineralogical Composition of Asteroid Ryugu with Ground-Based Observations
Constraining Mineralogical Composition of Asteroid Ryugu with Ground-Based Observations Lucille Le Corre1, Vishnu Reddy2, Juan A. Sanchez1, Driss Takir3, Ed A. Cloutis4, Audrey Thirouin5, Jian-Yang Li1, Seiji Sugita6, Eri Tatsumi6. 1Planetary Science Institute, Tucson, Arizona, USA 2Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA 3SETI Institute, Mountain View, CA, USA 4Department of Geography, University of Winnipeg, Winnipeg, Manitoba, Canada 5Lowell Observatory, Flagstaff, AZ, USA 6Dept. of Earth and Planetary Science, University of Tokyo, Tokyo, Japan In preparation for the arrival of the Japanese Space Agency’s (JAXA) Hayabusa2 sample return mission to near-Earth asteroid (NEA) (162173) Ryugu, we took the opportunity to characterize the target with a ground-based telescope. We observed Ryugu using the SpeX instrument in Prism mode on NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii, on July, 12 2016 when the asteroid was 18.87 visual magnitude, at a phase angle of 13.3°. The NIR spectra were used to constrain Ryugu’s surface composition, determine meteorite analogs and study spectral affinity to other asteroids. We also modeled its photometric properties using archival data. Using the Lommel-Seeliger model we computed the predicted flux for Ryugu at a wide range of viewing geometries as well as albedo quantities such as geometric albedo, phase integral, and spherical Bond albedo. Our computed albedo quantities are consistent with results from Ishiguro et al. (2014). In previous work, Ryugu’s visible spectrum revealed that it can be classified as a C-type object. In addition, not all previous ground-based observations of Ryugu detected the 0.7 µm absorption feature due to the presence of phyllosilicates. -
The Orbital Distribution of Near-Earth Objects Inside Earth’S Orbit
Icarus 217 (2012) 355–366 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The orbital distribution of Near-Earth Objects inside Earth’s orbit ⇑ Sarah Greenstreet a, , Henry Ngo a,b, Brett Gladman a a Department of Physics & Astronomy, 6224 Agricultural Road, University of British Columbia, Vancouver, British Columbia, Canada b Department of Physics, Engineering Physics, and Astronomy, 99 University Avenue, Queen’s University, Kingston, Ontario, Canada article info abstract Article history: Canada’s Near-Earth Object Surveillance Satellite (NEOSSat), set to launch in early 2012, will search for Received 17 August 2011 and track Near-Earth Objects (NEOs), tuning its search to best detect objects with a < 1.0 AU. In order Revised 8 November 2011 to construct an optimal pointing strategy for NEOSSat, we needed more detailed information in the Accepted 9 November 2011 a < 1.0 AU region than the best current model (Bottke, W.F., Morbidelli, A., Jedicke, R., Petit, J.M., Levison, Available online 28 November 2011 H.F., Michel, P., Metcalfe, T.S. [2002]. Icarus 156, 399–433) provides. We present here the NEOSSat-1.0 NEO orbital distribution model with larger statistics that permit finer resolution and less uncertainty, Keywords: especially in the a < 1.0 AU region. We find that Amors = 30.1 ± 0.8%, Apollos = 63.3 ± 0.4%, Atens = Near-Earth Objects 5.0 ± 0.3%, Atiras (0.718 < Q < 0.983 AU) = 1.38 ± 0.04%, and Vatiras (0.307 < Q < 0.718 AU) = 0.22 ± 0.03% Celestial mechanics Impact processes of the steady-state NEO population. -
Constraints on the Near-Earth Asteroid Obliquity Distribution from The
Astronomy & Astrophysics manuscript no. main c ESO 2017 September 4, 2017 Constraints on the near-Earth asteroid obliquity distribution from the Yarkovsky effect C. Tardioli1,?, D. Farnocchia2, B. Rozitis3, D. Cotto-Figueroa4, S. R. Chesley2, T. S. Statler5; 6, and M. Vasile1 1 Department of Mechanical & Aerospace Engineering, University of Strathclyde, Glasgow, G1 1XJ, UK 2 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA 3 School of Physical Sciences, The Open University, Milton Keynes, MK7 6AA, UK 4 Department of Physics and Electronics, University of Puerto Rico at Humacao, Humacao, 00792, Puerto Rico 5 Department of Astronomy, University of Maryland, College Park, MD, 20742, USA 6 Planetary Science Division, Science Mission Directorate, NASA Headquarters, Washington DC, 20546, USA September 4, 2017 ABSTRACT Aims. From lightcurve and radar data we know the spin axis of only 43 near-Earth asteroids. In this paper we attempt to constrain the spin axis obliquity distribution of near-Earth asteroids by leveraging the Yarkovsky effect and its dependence on an asteroid’s obliquity. Methods. By modeling the physical parameters driving the Yarkovsky effect, we solve an inverse problem where we test different simple parametric obliquity distributions. Each distribution re- sults in a predicted Yarkovsky effect distribution that we compare with a χ2 test to a dataset of 125 Yarkovsky estimates. Results. We find different obliquity distributions that are statistically satisfactory. In particular, among the considered models, the best-fit solution is a quadratic function, which only depends on two parameters, favors extreme obliquities, consistent with the expected outcomes from the YORP effect, has a 2:1 ratio between retrograde and direct rotators, which is in agreement with theoretical predictions, and is statistically consistent with the distribution of known spin axes of near-Earth asteroids. -
Detecting the Yarkovsky Effect Among Near-Earth Asteroids From
Detecting the Yarkovsky effect among near-Earth asteroids from astrometric data Alessio Del Vignaa,b, Laura Faggiolid, Andrea Milania, Federica Spotoc, Davide Farnocchiae, Benoit Carryf aDipartimento di Matematica, Universit`adi Pisa, Largo Bruno Pontecorvo 5, Pisa, Italy bSpace Dynamics Services s.r.l., via Mario Giuntini, Navacchio di Cascina, Pisa, Italy cIMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universits, UPMC Univ. Paris 06, Univ. Lille, 77 av. Denfert-Rochereau F-75014 Paris, France dESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1, 00044 Frascati (RM), Italy eJet Propulsion Laboratory/California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109 CA, USA fUniversit´eCˆote d’Azur, Observatoire de la Cˆote d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, Nice, France Abstract We present an updated set of near-Earth asteroids with a Yarkovsky-related semi- major axis drift detected from the orbital fit to the astrometry. We find 87 reliable detections after filtering for the signal-to-noise ratio of the Yarkovsky drift esti- mate and making sure the estimate is compatible with the physical properties of the analyzed object. Furthermore, we find a list of 24 marginally significant detec- tions, for which future astrometry could result in a Yarkovsky detection. A further outcome of the filtering procedure is a list of detections that we consider spurious because unrealistic or not explicable with the Yarkovsky effect. Among the smallest asteroids of our sample, we determined four detections of solar radiation pressure, in addition to the Yarkovsky effect. As the data volume increases in the near fu- ture, our goal is to develop methods to generate very long lists of asteroids with reliably detected Yarkovsky effect, with limited amounts of case by case specific adjustments.