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BENNU from OSIRIS-Rex APPROACH and PRELIMINARY SURVEY OBSERVATIONS
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1956.pdf VNIR AND TIR SPECTRAL CHARACTERISTICS OF (101955) BENNU FROM OSIRIS-REx APPROACH AND PRELIMINARY SURVEY OBSERVATIONS. V. E. Hamilton1, A. A. Simon2, P. R. Christensen3, D. C. Reuter2, D. N. Della Giustina4, J. P. Emery5, R. D. Hanna6, E. Howell4, H. H. Kaplan1, B. E. Clark7, B. Rizk4, D. S. Lauretta4, and the OSIRIS-REx Team, 1Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302 ([email protected]), 2NASA Goddard Space Flight Center, Greenbelt, MD, 3School of Earth & Space Ex- ploration, Arizona State University, Tempe, AZ 85287, 4Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, 5Dept. Earth & Planetary Science, University of Tennessee, Knoxville, TN 37996, 6University of Texas, Austin, TX, 78712, 7Dept. Physics & Astronomy, Ithaca College, Ithaca, NY 14850. Introduction: Visible to near infrared (VNIR) and generation and application of a photometric model, thermal infrared (TIR) spectrometers onboard the Ori- production of bolometric Bond albedo, reflectance gins, Spectral Interpretation, Resource Identification, factor spectra, and the calculation of spectral indices. Security–Regolith Explorer (OSIRIS-REx) spacecraft For OTES, this includes deriving emissivity spectra have revealed evidence of hydrated phases across the and temperature information with emissivity being an surface of asteroid (101955) Bennu. Here we describe input into a linear least squares mixing model and a spectral features identified -
Observation of Near-Earth Object (1566) Icarus and the Split Candidate 2007 MK6
PPS07-P07 JpGU-AGU Joint Meeting 2017 Observation of near-earth object (1566) Icarus and the split candidate 2007 MK6 *Seitaro Urakawa1, Katsutoshi Ohtsuka2, Shinsuke Abe3, Daisuke Kinoshita4, Hidekazu Hanayama 5, Takeshi Miyaji5, Shin-ichiro Okumura1, Kazuya Ayani6, Syouta Maeno6, Daisuke Kuroda5, Akihiko Fukui5, Norio Narita5,7,8, George HASHIMOTO9, Yuri SAKURAI9, Sayuri Nakamura9, Jun Takahashi10, Tomoyasu Tanigawa11, Otabek Burhonov12, Kamoliddin Ergashev12, Takashi Ito5, Fumi Yoshida5, Makoto Watanabe13, Masataka Imai14, Kiyoshi Kuramoto14, Tomohiko Sekiguchi15 , MASATERU ISHIGURO16 1. Japan Spaceguard Association, 2. Tokyo Meteor Network, 3. Nihon University, 4. National Central University, 5. National Astronomical Observatory of Japan, 6. Bisei Observatory, 7. Astrobiology Center, 8. University of Tokyo, 9. Okayama University, 10. University of Hyogo, 11. Sanda Shounkan Highschool, 12. Ulugh Beg Astronomical Institute Uzbekistan Academy of Science , 13. Okayama University of Science, 14. Hokkaido University, 15. Hokkaido University of Education, 16. Seoul National University Background & Aim: A numerical simulation proposes that the origin of near-Earth object 2007 MK6 (hereafter, MK6) is a near-Earth object (1566) Icarus (hereafter, Icarus) [1]. In addition to it, the orbital parameters of the daytime Taurid-Perseid meteor swarm are in good agreement with those of Icarus. Thus, it is considered that MK6 is split from the parent object Icarus by a rotational fission and/or an impact event, and the produced dust became to the daytime Taurid-Perseid meteor swarm. To confirm such a hypothesis, we need to obtain the observational evidence that the color indices of Icarus and MK6 are same. Moreover, if MK6 split by the rotational fission due to the YORP effect, the rotation period of Icarus would be shorten compared with the past rotation period. -
Bennu: Implications for Aqueous Alteration History
RESEARCH ARTICLES Cite as: H. H. Kaplan et al., Science 10.1126/science.abc3557 (2020). Bright carbonate veins on asteroid (101955) Bennu: Implications for aqueous alteration history H. H. Kaplan1,2*, D. S. Lauretta3, A. A. Simon1, V. E. Hamilton2, D. N. DellaGiustina3, D. R. Golish3, D. C. Reuter1, C. A. Bennett3, K. N. Burke3, H. Campins4, H. C. Connolly Jr. 5,3, J. P. Dworkin1, J. P. Emery6, D. P. Glavin1, T. D. Glotch7, R. Hanna8, K. Ishimaru3, E. R. Jawin9, T. J. McCoy9, N. Porter3, S. A. Sandford10, S. Ferrone11, B. E. Clark11, J.-Y. Li12, X.-D. Zou12, M. G. Daly13, O. S. Barnouin14, J. A. Seabrook13, H. L. Enos3 1NASA Goddard Space Flight Center, Greenbelt, MD, USA. 2Southwest Research Institute, Boulder, CO, USA. 3Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA. 4Department of Physics, University of Central Florida, Orlando, FL, USA. 5Department of Geology, School of Earth and Environment, Rowan University, Glassboro, NJ, USA. 6Department of Astronomy and Planetary Sciences, Northern Arizona University, Flagstaff, AZ, USA. 7Department of Geosciences, Stony Brook University, Stony Brook, NY, USA. 8Jackson School of Geosciences, University of Texas, Austin, TX, USA. 9Smithsonian Institution National Museum of Natural History, Washington, DC, USA. 10NASA Ames Research Center, Mountain View, CA, USA. 11Department of Physics and Astronomy, Ithaca College, Ithaca, NY, USA. 12Planetary Science Institute, Tucson, AZ, Downloaded from USA. 13Centre for Research in Earth and Space Science, York University, Toronto, Ontario, Canada. 14John Hopkins University Applied Physics Laboratory, Laurel, MD, USA. *Corresponding author. E-mail: Email: [email protected] The composition of asteroids and their connection to meteorites provide insight into geologic processes that occurred in the early Solar System. -
1922MNRAS..82..149G Jan. 1922. Long-Period Inequalities In
Jan. 1922. Long-Period Inequalities in Movements of Asteroids. 149 In the case = an integer ~ is a multiple of and the solutions X2 X2 a1 1922MNRAS..82..149G with period nearly equal to — may also be regarded as periodic solution» Ai with period nearly equal to —-. A . But we have not been able (in the case when ^ is an integer) to A2 prove the existence of periodic solutions with period ^ which are not A2 • • • 2 TT at the same time periodic with period nearly equal to — . Ax Note.—The above work was completed in 1920 November, before the appearance of Moulton’s Periodic Orbits. The details of the exist- ence proofs are different from those of Buck, and it is hoped that they may be of interest. In Buck’s paper, which apparently was completed in 1912 or earlier, the equations of motion are transformed and the jacobians take a relatively simple form. In this paper only two of the families of periodic orbits treated by Buck are discussed. A full account of the other families, and also of the actual development in series of the periodic solutions, is given in Back’s paper. On Long-Period Inequalities in the Movements of Asteroids ivhose Mean Motions are nearly half that of Mars. By Wt M. H. Greaves, B. A., Isaac Newton Student in the University of Cambridge. (Communicated by Professor H. F. Baker.) In the ordinary theory of the movements of the planets as developed by Laplace and Le Verrier, the equations of motion are integrated by a method of successive approximation with regard to the masses. -
107 Minor Planet Bulletin 37(2010) LIGHTCURVE PHOTOMETRY of 112 IPHIGENIA Stefan Cikota Physik-Institut, Universität Zürich, W
107 LIGHTCURVE PHOTOMETRY OF 112 IPHIGENIA Stefan Cikota Physik-Institut, Universität Zürich, Winterthurerstrasse 190, CH-8057 Zürich, SWITZERLAND and Observatorio Astronomico de Mallorca 07144 Costitx, Mallorca, Illes Balears, SPAIN [email protected] Aleksandar Cikota Physik-Institut, Universität Zürich, CH-8057 Zürich, SWITZERLAND and Observatorio Astronomico de Mallorca MINOR PLANET LIGHTCURVE ANALYSIS OF 07144 Costitx, Mallorca, Illes Balears, SPAIN 347 PARIANA AND 6560 PRAVDO (Received: 19 March) Peter Caspari BDI Observatory PO Box 194 Regents Park The main-belt asteroid 112 Iphigenia was observed over NSW 2143, AUSTRALIA 6 nights between 2007 December 9 and December 14 at [email protected] the Observatorio Astronomico de Mallorca (620). From the resulting data, we determined a synodic rotation (Received: 15 January Revised: 22 February) period of 31.385 ± 0.006 h and lightcurve amplitude of 0.30 ± 0.02 mag. Minor planet 347 Pariana was observed in 2009 July and again in 2009 August and September resulting in two 122 Iphigenia was tracked over 6 nights between 2007 December complete lightcurves both with a rotational period 9 and December 14 with one, and sometimes two, identical estimate of 4.052 ± 0.002 h and amplitude of 0.5 mag. telescopes (0.30-m f/9 Schmidt-Cassegrain) located at the These data were combined with data from previous Observatorio Astronomico de Mallorca in Spain. Both were apparitions to produce estimates for a sidereal period, equipped with an SBIG STL-1001E CCD camera. Image spin axis, and shape model. Minor planet 6560 Pravdo acquisition and calibration were performed using Maxim DL. All was observed over nine nights in 2009 June and July 1593 images were unfiltered and had exposures of 60 seconds. -
Asteroid 1566 Icarus's Size, Shape, Orbit, and Yarkovsky Drift from Radar
Draft version January 16, 2017 Preprint typeset using LATEX style emulateapj v. 5/2/11 ASTEROID 1566 ICARUS'S SIZE, SHAPE, ORBIT, AND YARKOVSKY DRIFT FROM RADAR OBSERVATIONS Adam H. Greenberg University of California, Los Angeles, CA Jean-Luc Margot University of California, Los Angeles, CA Ashok K. Verma University of California, Los Angeles, CA Patrick A. Taylor Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA Shantanu P. Naidu Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA Marina. Brozovic Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA Lance A. M. Benner Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA Draft version January 16, 2017 ABSTRACT Near-Earth asteroid (NEA) 1566 Icarus (a = 1:08 au, e = 0:83, i = 22:8◦) made a close approach to Earth in June 2015 at 22 lunar distances (LD). Its detection during the 1968 approach (16 LD) was the first in the history of asteroid radar astronomy. A subsequent approach in 1996 (40 LD) did not yield radar images. We describe analyses of our 2015 radar observations of Icarus obtained at the Arecibo Observatory and the DSS-14 antenna at Goldstone. These data show that the asteroid is a moderately flattened spheroid with an equivalent diameter of 1.44 km with 18% uncertainties, resolving long-standing questions about the asteroid size. We also solve for Icarus' spin axis orientation (λ = 270◦ ± 10◦; β = −81◦ ± 10◦), which is not consistent with the estimates based on the 1968 lightcurve observations. Icarus has a strongly specular scattering behavior, among the highest ever measured in asteroid radar observations, and a radar albedo of ∼2%, among the lowest ever measured in asteroid radar observations. -
Deleoneulalia.Pdf
Publication Year 2016 Acceptance in OA@INAF 2020-05-13T12:53:09Z Title Visible spectroscopy of the Polana-Eulalia family complex: Spectral homogeneity Authors de León, J.; Pinilla-Alonso, N.; Delbo, M.; Campins, H.; Cabrera-Lavers, A.; et al. DOI 10.1016/j.icarus.2015.11.014 Handle http://hdl.handle.net/20.500.12386/24794 Journal ICARUS Number 266 Visible Spectroscopy of the Polana-Eulalia Family Complex: Spectral Homogeneity J. de Le´ona,b, N. Pinilla-Alonsoc, M. Delb´od, H. Campinse, A. Cabrera-Laversf,a, P. Tangad, A. Cellinog, P. Bendjoyad, J. Licandroa,b, V. Lorenzih, D. Moratea,b, K. Walshi, F. DeMeoj, Z. Landsmane aInstituto de Astrof´ısica de Canarias, C/V´ıaL´actea s/n, 38205, La Laguna, Spain bDepartment of Astrophysics, University of La Laguna, 38205, Tenerife, Spain cDepartment of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, USA dLaboratoire Lagrange, Observatoire de la Co^te d'Azur, Nice, France eof Central Florida, Physics Department, PO Box 162385, Orlando, FL 32816.2385, USA fGTC Project, 38205 La Laguna, Tenerife, Spain gINAF, Osservatorio Astrofisico di Torino, Pino Torinese, Italy hFundacin Galileo Galilei - INAF, La Palma, Spain iSouthwest Research Institute, Boulder, CO, USA jMIT, Cambridge, MA, USA Abstract Insert abstract text here Keywords: Asteroids, composition, Spectroscopy, Asteroids, dynamics 1. Introduction The main asteroid belt, located between the orbits of Mars and Jupiter, is considered the principal source of near-Earth asteroids (Bottke et al., 2002). In particular the region bounded by two major resonances, the ν6 secular resonance near 2.15 AU that marks the inner border of the main belt, and the 3:1 mean motion resonance with Jupiter at 2.5 AU. -
Arecibo Radar Observations of 14 High-Priority Near-Earth Asteroids in CY2020 and January 2021 Patrick A
Arecibo Radar Observations of 14 High-Priority Near-Earth Asteroids in CY2020 and January 2021 Patrick A. Taylor (LPI, USRA), Anne K. Virkki, Flaviane C.F. Venditti, Sean E. Marshall, Dylan C. Hickson, Luisa F. Zambrano-Marin (Arecibo Observatory, UCF), Edgard G. Rivera-Valent´ın, Sriram S. Bhiravarasu, Betzaida Aponte-Hernandez (LPI, USRA), Michael C. Nolan, Ellen S. Howell (U. Arizona), Tracy M. Becker (SwRI), Jon D. Giorgini, Lance A. M. Benner, Marina Brozovic, Shantanu P. Naidu (JPL), Michael W. Busch (SETI), Jean-Luc Margot, Sanjana Prabhu Desai (UCLA), Agata Rozek˙ (U. Kent), Mary L. Hinkle (UCF), Michael K. Shepard (Bloomsburg U.), and Christopher Magri (U. Maine) Summary We propose the continuation of the long-running project R3037 to physically and dynamically characterize the population of near-Earth asteroids with the Arecibo S-band (2380 MHz; 12.6 cm) planetary radar system. The objectives of project R3037 are to: (1) collect high-resolution radar images of and (2) report ultra-precise radar astrometry for the strongest predicted radar targets for the 2020 calendar year plus early January 2021. Such images will be used for three-dimensional shape modeling as the data sets allow. These observations will be carried out as part of the NASA- funded Arecibo planetary radar program, Grant No. 80NSSC19K0523, to PI Anne Virkki (Arecibo Observatory, University of Central Florida) with Patrick Taylor as Institutional PI at the Lunar and Planetary Institute (Universities Space Research Association). Background Radar is arguably the most powerful Earth-based technique for post-discovery physical and dynamical characterization of near-Earth asteroids (NEAs) and plays a crucial role in the nation’s planetary defense initiatives led through the NASA Planetary Defense Coordination Office. -
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. -
SOLAR ECLIPSE NEWSLETTER SOLAR ECLIPSE March 2002 NEWSLETTER
Volume 7, Issue 3 SOLAR ECLIPSE NEWSLETTER SOLAR ECLIPSE March 2002 NEWSLETTER SUBSCRIBING TO The sole Newsletter dedicated to Solar Eclipses THE SOLAR Dear All, gathered form the SEML but as well ECLIPSE MAILING form other solar eclipse related We are getting closer to the next solar sources. If you want to contribute, LIST eclipse event. Many of you booked in the please send us a message. THE SOLAR ECLIPSE meanwhile a trip to Mexico for the annular MAILINGING LISTLIST ISIS MAIMAIN- eclipse of 10 June 2002. Some of you will As you will notice, Glenn Schneider TAINED BY THE LIST make attempts to observe from the ocean has been put in the solar eclipse spot- by boat or ship. light. We hope we can highlight some OWNER PATRICK POITE- one else from the SEML soon. We VIN AND WITH THE SUP- Joanne and I booked as well the flights and thought it was a nice idea. PORT OF JAN VAN GESTEL will travel around as we did before: Public transport, back pack and as cheap as pos- Barrie Jones from the Open University HOW TO SUBSCRIBE: sible accommodations. We are sure we will of Milton Keynes, has been promoted ININ THETHE BODYBODY OFOF THETHE meet many of you in Puerto Vallarta. It will to Professor in Astronomy. Congratu- MES SAGE TO be the Mecca of the 11 June 2002 eclipse. lations from all of us. Barrie did some [email protected]@Aula.com SUSUB- Be there!!! great work on shadow bands studies. For us, he is as well the wonderful SCRIBE SOLARECLIPSES But after June it will be soon December. -
Imaging of Near-Earth Asteroids
Imaging of Near-Earth Asteroids. Michael C. Nolan, Arecibo Observatory / Cornell University. [email protected] (787) 878-2612 ext 212 Lance A. M. Benner (Jet Propulsion Laboratory / California Institute of Technology) Marina Brozovič (Jet Propulsion Laboratory / California Institute of Technology) Ellen S. Howell (Arecibo Observatory / Cornell University) Jean-Luc Margot (UCLA) Abstract As remnants of accretion, building blocks of planets, space resources and potential impactors, the asteroids offer insights to solar system formation and evolution. Recent results show that this population is extremely diverse, compositionally, texturally and structurally. As a result, spacecraft cannot explore the population of asteroids in a reasonable time or at a reasonable cost without guidance from Earth-based reconnaissance. Compositional variation can be studied using remote-sensing spectroscopic techniques, either ground-based or from general-purpose space-based telescopes such as HST and JWST. Study of the textural and structural properties of asteroids requires imaging and shape determination. In addition, the largest uncertainties in orbit determination arise from non-gravitational forces, such as the Yarkovsky effect, that depend on the detailed shapes of asteroids. This shape determination can be done crudely using visible lightcurves and in detail using direct imaging (generally using adaptive optics), interferometric and radar techniques. Of these, only ground-based radar using the Arecibo and Goldstone radar systems has been routinely used for asteroid imaging, typically yielding shapes with tens to hundreds of pixels across a diameter and an absolute size accuracy of 5% or better. Other groundbased techniques are unlikely to achieve this level of precision in the upcoming decade, and space-based techniques will visit no more than a few targets. -
Asteroids and Comets: U.S
Columbia Law School Scholarship Archive Faculty Scholarship Faculty Publications 1997 Asteroids and Comets: U.S. and International Law and the Lowest-Probability, Highest Consequence Risk Michael B. Gerrard Columbia Law School, [email protected] Anna W. Barber Follow this and additional works at: https://scholarship.law.columbia.edu/faculty_scholarship Part of the Environmental Law Commons, and the International Law Commons Recommended Citation Michael B. Gerrard & Anna W. Barber, Asteroids and Comets: U.S. and International Law and the Lowest- Probability, Highest Consequence Risk, 6 N.Y.U. ENVTL. L. J. 4 (1997). Available at: https://scholarship.law.columbia.edu/faculty_scholarship/697 This Article is brought to you for free and open access by the Faculty Publications at Scholarship Archive. It has been accepted for inclusion in Faculty Scholarship by an authorized administrator of Scholarship Archive. For more information, please contact [email protected]. COLLOQUIUM ARTICLES ASTEROIDS AND COMETS: U.S. AND INTERNATIONAL LAW AND THE LOWEST-PROBABILITY, HIGHEST ICONSEQUENCE RISK MICHAEL B. GERRARD AND ANNA W. BARBER* INTRODUCrION Asteroids' and comets2 pose unique policy problems. They are the ultimate example of a low probability, high consequence event: no one in recorded human history is confirmed to have ever died from an asteroid or a comet, but the odds are that at some time in the next several centuries (and conceivably next year) an asteroid or a comet will cause mass localized destruction and that at some time in the coming half million years (and con- ceivably next year), an asteroid or a comet will kill several billion people.