Table of Contents

Total Page:16

File Type:pdf, Size:1020Kb

Table of Contents Table of Contents Preface 1–3 T. J. JOPEK, G. B. VALSECCHI AND CL. FROESCHLE´ / Possible meteoroid streams associated with (69230) Hermes and 2002 SY50 5–10 IWAN P. WILLIAMS, G. O. RYABOVA, A. P. BATURIN AND A. M. CHERNITSOV / Are Asteroid 2003 EH1 and Comet C/1490 Y1 Dynamically Related? 11–18 PAUL WIEGERT AND PETER BROWN / The problem of linking minor meteor showers to their parent bodies: initial con- siderations 19–26 JU¨ RGEN RENDTEL / Evolution of the Geminids Observed Over 60 Years 27–32 A. R. HILDEBR, R. D. CARDINAL, K. A. CARROLL, D. R. FABER, E. F. TEDESCO, J. M. MATTHEWS, R. KUSCHNIG, G. A. H. WALK- ER, B. GLADMAN, J. PAZDER, P. G. BROWN, S. M. LARSON, S. P. WORDEN, B. J. WALLACE, P. W. CHODAS, K. MUINONEN AND A. CHENG / Advantages of Searching for Asteroids from Low Earth Orbit: The Neossat Mission 33–40 S. STARCZEWSKI AND T. J. JOPEKDynamical Relation of Me- teorids to Comets and Asteroids 41–47 JUN-ICHI WATANABE / Meteor Streams and Comets 49–61 SANG-HYEON AHN / Meteoric Activities of the Last Millennium 63–68 JA´ N SVORE, LUBOSˇ NESLUSˇ AN, ZUZANA KAUCHOVA´ AND VLA- DIMI´ R PORUBAN / A Fine Structure of the Perseid Me- teoroid Stream 69–74 J. VAUBAILLON, P. LAMY AND L. JORDA / Meteoroid Streams Associated to Comets 9P/TEMPEL 1 and 67P/CHUR- YUMOV-GERASIMENKO 75–80 PAUL WIEGERT AND PETER BROWN / The Core of the Quadrantid Meteoroid Stream is Two Hundred Years Old 81–88 LARS P. DYRUD, KELLY DENNEY, JULIO URBINA, DIEGO JAN- CHES, ERHAN KUDEKI AND STEVE FRANKE / The Meteor Flux: It Depends How You Look 89–100 CSILLA SZASZ, JOHAN KERO, ASTA PELLINEN-WANNBERG, JOHN D. MATHEWS, NICK J. MITCHELL AND WERNER SINGER / Latitudinal Variations of Diurnal Meteor Rates 101–107 V. DIKAREV, E. GRU¨ N, J. BAGGALEY, D. GALLIGAN, M. LAND- GRAF AND R. JEHN / Modeling the Sporadic Meteoroid Background Cloud 109–122 H. MCNAMARA, R. SUGGS, B. KAUFFMAN, J. JONES, W. COOKE AND S. SMITH / Meteoroid Engineering Model (MEM): A Meteoroid Model For The Inner Solar System 123–139 DANIELLE E. MOSER AND WILLIAM J. COOKE / MSFC Stream Model Preliminary Results: Modeling Recent Leonid and Perseid Encounters 141–153 V. SIDOROV, S. KALABANOV, S. SIDOROVA AND I. FILIN / Micro- shower Structure of the Meteor Complex 155–164 V. SIDOROV, S. KALABANOV, S. SIDOROVA, I. FILIN AND T. FILI- MONOVA / Associations of Meteor Microshowers or as the Kazan Radar ‘‘Sees’’ Radiants on Northern Celestial Hemisphere 165–179 J. TO´ TH AND J. KLAKA / Fragmentation of Leonids in space and a model of spatial distribution of meteoroids within the Leo- nid stream 181–186 R. L. HAWKES AND R. A. EATON / Mass Flux of Asteroidal Origin Meteoroids on Periodic Comet Nuclei 187–195 W. J. BAGGALEY / Interstellar dust in the solar system 197–209 R. SRAMA, A. SROWIG, M. RACHEV, E. GRU¨ N, S. KEMPF, G. MOR- AGAS-KLOSTERMEYER T. CONLON, D.HARRIS, S.AUER, A. GLASMACHERS, S. HELFERT, H. LINNEMANN, AND V. TSCHERNJAWSKI / Development of an Advanced Dust Telescope 211–220 R. J. WERYK AND P. BROWN / A Search for Interstellar Meteoroids Using the Canadian Meteor Orbit Radar (CMOR) 221–227 SVITLANA V. KOLOMIYETS AND BORIS L. KASHCHEYEV / Com- plex of Meteoroid Orbits with Eccentricities Near 1 and Higher 229–235 L. A. ROGERS, K. A. HILL AND R. L. HAWKES / Optical Predictions for High Geocentric Velocity Meteors 237–244 JII´ BOROVIKA / Elemental Abundances in Leonid and Perseid Meteoroids 245–253 DETLEF KOSCHNY, JORGE DIAZ DEL RIO, RODRIGUE PIBERNE, MAREK SZUMLAS, JOE ZENDER AND ANDRE´ KNO¨ FEL / Radiants of the Leonids 1999 and 2001 Obtained by LLTV Systems Using Automatic Software Tools 255–263 SHINSUKE ABE, NOBORU EBIZUKA, HIDEYUKI MURAYAMA, KATSUHITO OHTSUKA, SATORU SUGIMOTO, MASA-YUKI YAMAMOTO, HAJIME YANO, JUN-ICHI WATANABE AND JII´ BOROVIKA / Video and Photographic Spectroscopy of 1998 and 2001 Leonid Persistent Trains from 300 to 930 nm 265–277 MASA-YUKI YAMAMOTO, MASAYUKI TODA, YOSHIHIRO HIGA, KOUJI MAEDA AND JUN-ICHI WATANABE / Altitudinal Distribution Of 20 Persistent Meteor Trains: Estimates Derived from Metro Campaign Archives 279–287 A. J. FALOON, J. D. THALER AND R. L. HAWKES / Searching for Light Curve Evidence of Meteoroid Structure and Fragmentation 289–295 M. D. CAMPBELL-BROWN / Arietid Meteor Orbits Measurements 297–301 OLGA POPOVA / Meteoroid ablation models 303–319 FRANS J. M. RIETMEIJER / Interplanetary Dust and Carbonaceous Meteorites: Constraints on Porosity, Mineralogy and Chemistry of Meteors from Rubble-Pile Planetesimals 321–338 PETER JENNISKENS, PAUL WERCINSKI, JOE OLEJNICZAK, GEORGE RAICHE, DEAN KONTINOS, GARY ALLEN, PRA- SUN N. DESAI, DOUG REVELLE, JASON HATTON, RICHARD L. BAKER, RAY W. RUSSELL, MIKE TAYLOR AND FRANS RIETMEIJER / Preparing For Hyperseed MAC: An Obser- ving Campaign To Monitor The Entry Of The Genesis Sample Return Capsule 339–360 GEORGE J. FLYNN / Physical Properties of Meteorites and Inter- planetary Dust Particles: Clues to the Properties of the Meteors and their Parent Bodies 361–374 J. M. TRIGO-RODRI´ GUEZ, J. LLORCA, J. BOROVIKA AND J. FAB- REGAT / Spectroscopy of a Geminid Fireball: Its Similarity to Cometary Meteoroids and the Nature of its Parent Body 375–387 MARTIN BEECH AND MEGAN HARGROVE / Classical Meteor Light Curve Morphology 389–394 D. YU. KHANUKAEVA AND G. A. TIRSKIY / A Model of Single and Fragmenting Meteoroid Interaction with Isothermal and Non-Isothermal Atmosphere 395–402 K. A. HILL, L. A. ROGERS AND R. L. HAWKES / Sputtering and High Altitude Meteors 403–412 LAURA SCHAEFER AND BRUCE FEGLEY JR.Application of an Equilibrium Vaporization Model to the Ablation of Chondritic and Achondritic Meteoroids 413–423 APOSTOLOS A. CHRISTOU / Predicting Martian and Venusian Meteor Shower Activity 425–431 D. YU. KHANUKAEVA / Calculation of Variable Drag and Heat- Transfer Coefficients in Meteoric Physics Equations 433–439 D. O. REVELLE / Recent Advances in Bolide Entry Modeling: A Bolide Potpourri 441–476 PAVEL SPURN AND ZDENEK CEPLECHA / Fragmentation Model Analysis of EN270200 Fireball 477–487 M. D. CAMPBELL-BROWN AND A. HILDEBRAND / A New Analysis of Fireball Data from the Meteorite Observation and Re- covery Project (MORP) 489–499 WAYNE N. EDWARDS, PETER G. BROWN AND DOUGLAS O. RE- VELLE / Bolide Energy Estimates from Infrasonic Mea- surements 501–512 G. A. TIRSKIY AND D.YU. KHANUKAEVA / The Modeling of Bo- lide Terminal Explosions 513–520 M. D. CAMPBELL-BROWN / Optical Observations of Meteors 521–531 WESLEY R. SWIFT, ROBERT M. SUGGS AND WILLIAM J. COOKE / Meteor44 Video Meteor Photometry 533–540 PETER S. GURAL, PETER M. JENNISKENS AND GEORGE VARROS / Results from the AIM-IT meteor tracking system 541–552 J. M. TRIGO-RODRI´ GUEZ, A. J. CASTRO-TIRADO, J. LLORCA, J. FABREGAT, V. J. MARTI´ NEZ, V. REGLERO, M. JELI´ NEK, P. KUBA´ NEK, T. MATEO AND A. DE UGARTE POSTIGO / The Development of the Spanish Fireball Network Using a New All-Sky CCD System 553–567 PAVEL SPURN, JII´ BOROVIKA AND PAVEL KOTEN / Multi-Instru- ment Observations of Bright Meteors in the Czech Republic 569–578 N. KAISER, P. BROWN AND R. L. HAWKES / Optical Trail Width Measurements of Faint Meteors 579–586 R. L. HAWKES, P. G. BROWN, N. R. KAISER, A. J. FALOON, K. A. HILL AND L. A. ROGERS / High Spatial and Temporal Re- solution Optical Search for Evidence of Meteoroid Frag- mentation 587–593 Y. FUJIWARA, M. UEDA, M. SUGIMOTO, T. SAGAYAMA AND S. ABE / TV Observation of the Daytime Meteor Shower; the Arietids 595–600 W. J. BAGGALEY AND J. GRANT / Techniques for Measuring Radar Meteor Speeds 601–615 P. BROWN, J. JONES, R. J. WERYK AND M. D. CAMPBELL-BROWN / The Velocity Distribution of Meteoroids at the Earth as Measured by the Canadian Meteor Orbit Radar (CMOR) 617–626 ASTA PELLINEN-WANNBERG, EDMOND MURAD, GUDMUND WANNBERG AND ASSAR WESTMAN / The Hyperthermal Ionization and High Absolute Meteor Velocities Observed with HPLA Radars 627–632 JOHAN KERO, CSILLA SZASZ, ASTA PELLINEN-WANNBERG, GUDMUND WANNBERG AND ASSAR WESTMAN / Power Fluctuations in Meteor Head Echoes Observed with the EISCAT VHF Radar 633–638 K. DREW, P. G. BROWN, S. CLOSE AND D. DURAND / Meteoroid Bulk Density Determination Using Radar Head Echo Observa- tions 639–645 W. J. BAGGALEY AND J. GRANT / Radar Measurements of Me- teoroid Decelerations 647–654 W. J. BAGGALEY AND J. GRANT / Radar Measurements of Macro Fragmentation in Meteoroids 655–662 W. J. BAGGALEY, G. E. PLANK, L. TOMLINSON AND J. GRANT / Radar Campaign to Determine the Dependence of Initial Radii of Meteor Plasma Trains on Trajectory and Orbit 663–669 W. K. HOCKING / Experimental Radar Studies of Anisotropic Diffusion of High Altitude Meteor Trails 671–679 P. PECINA, D. PECINOVA´ , V. PORUBAN AND J. TOTH / Radar Ob- servations of Taurid Complex Meteor Showers in 2003: Activity and Mass Distribution 681–688 D. PECINOVA´ AND P. PECINA / Radar Meteors Range Distribution and Some Parameters of Meteoroids: Application to Per- seids and b Taurids Showers 689–696 V. PORUBAN, L. KORNOSˇ AND I.P. WILLIAMS / Associations be- tween asteroids and meteoroid streams 697–711 A. R. WEBSTER AND J. JONES / Single and Multi-Station Radar Observations of the Geminid/Sextantid Meteor Stream System 713–721 PETER JENNISKENS / On the Future Prospects of Meteor Detec- tions (Invited Review) 723–732.
Recommended publications
  • Temperature-Induced Effects and Phase Reddening on Near-Earth Asteroids
    Planetologie Temperature-induced effects and phase reddening on near-Earth asteroids Inaugural-Dissertation zur Erlangung des Doktorgrades der Naturwissenschaften im Fachbereich Geowissenschaften der Mathematisch-Naturwissenschaftlichen Fakultät der Westfälischen Wilhelms-Universität Münster vorgelegt von Juan A. Sánchez aus Caracas, Venezuela -2013- Dekan: Prof. Dr. Hans Kerp Erster Gutachter: Prof. Dr. Harald Hiesinger Zweiter Gutachter: Dr. Vishnu Reddy Tag der mündlichen Prüfung: 4. Juli 2013 Tag der Promotion: 4. Juli 2013 Contents Summary 5 Preface 7 1 Introduction 11 1.1 Asteroids: origin and evolution . 11 1.2 The asteroid-meteorite connection . 13 1.3 Spectroscopy as a remote sensing technique . 16 1.4 Laboratory spectral calibration . 24 1.5 Taxonomic classification of asteroids . 31 1.6 The NEA population . 36 1.7 Asteroid space weathering . 37 1.8 Motivation and goals of the thesis . 41 2 VNIR spectra of NEAs 43 2.1 The data set . 43 2.2 Data reduction . 45 3 Temperature-induced effects on NEAs 55 3.1 Introduction . 55 3.2 Temperature-induced spectral effects on NEAs . 59 3.2.1 Spectral band analysis of NEAs . 59 3.2.2 NEAs surface temperature . 59 3.2.3 Temperature correction to band parameters . 62 3.3 Results and discussion . 70 4 Phase reddening on NEAs 73 4.1 Introduction . 73 4.2 Phase reddening from ground-based observations of NEAs . 76 4.2.1 Phase reddening effect on the band parameters . 76 4.3 Phase reddening from laboratory measurements of ordinary chondrites . 82 4.3.1 Data and spectral band analysis . 82 4.3.2 Phase reddening effect on the band parameters .
    [Show full text]
  • Many Binaries Among Neas D
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Many binaries among NEAs D. Polishook a,b,* and N. Brosch b a Department of Geophysics and Planetary Sciences, Tel-Aviv University, Israel. b The Wise Observatory and the School of Physics and Astronomy, Tel-Aviv University, Israel. * Corresponding author: David Polishook, [email protected] The number of binary asteroids in the near-Earth region might be significantly higher than expected. While Bottke and Melosh (1996) suggested that about 15% of the NEAs are binaries, as indicated from the frequency of double craters, and Pravec and Harris (2000) suggested that half of the fast-rotating NEAs are binaries, our recent study of Aten NEA lightcurves shows that the fraction of binary NEAs might be even higher than 50%. We found two asteroids with asynchronous binary characteristics such as two additive periods and fast rotation of the primary fragment. We also identified three asteroids with synchronous binary characteristics such as amplitude higher than one magnitude, U-shaped lightcurve maxima and V-shaped lightcurve minima. These five binaries were detected out of a sample of eight asteroids observed, implying a 63% binarity frequency. Confirmation of this high binary population requires the study of a larger representative sample. However, any mitigation program that requires the deflection or demise of a potential impactor will have to factor in the possibility that the target is a binary or multiple asteroid system. Introduction This technique is best used for binaries with NEAs mitigation techniques are asynchronous periods where the different suggested with reference to objects size, frequencies are easily noticed.
    [Show full text]
  • Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations Q ⇑ F
    Icarus 221 (2012) 1130–1161 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations q ⇑ F. Marchis a,g, , J.E. Enriquez a, J.P. Emery b, M. Mueller c, M. Baek a, J. Pollock d, M. Assafin e, R. Vieira Martins f, J. Berthier g, F. Vachier g, D.P. Cruikshank h, L.F. Lim i, D.E. Reichart j, K.M. Ivarsen j, J.B. Haislip j, A.P. LaCluyze j a Carl Sagan Center, SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, USA b Earth and Planetary Sciences, University of Tennessee, 306 Earth and Planetary Sciences Building, Knoxville, TN 37996-1410, USA c SRON, Netherlands Institute for Space Research, Low Energy Astrophysics, Postbus 800, 9700 AV Groningen, Netherlands d Appalachian State University, Department of Physics and Astronomy, 231 CAP Building, Boone, NC 28608, USA e Observatorio do Valongo, UFRJ, Ladeira Pedro Antonio 43, Rio de Janeiro, Brazil f Observatório Nacional, MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro, RJ, Brazil g Institut de mécanique céleste et de calcul des éphémérides, Observatoire de Paris, Avenue Denfert-Rochereau, 75014 Paris, France h NASA, Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000, USA i NASA, Goddard Space Flight Center, Greenbelt, MD 20771, USA j Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27514, USA article info abstract Article history: We collected mid-IR spectra from 5.2 to 38 lm using the Spitzer Space Telescope Infrared Spectrograph Available online 2 October 2012 of 28 asteroids representative of all established types of binary groups.
    [Show full text]
  • The Yarkovsky and YORP Effects
    The Yarkovsky and YORP Effects David Vokrouhlicky´ Institute of Astronomy, Charles University, Prague William F. Bottke Department of Space Studies, Southwest Research Institute, Boulder Steven R. Chesley Jet Propulsion Laboratory, California Institute of Technology, Pasadena Daniel J. Scheeres Aerospace Engineering Sciences, University of Colorado, Boulder Thomas S. Statler Astrophysical Institute, Ohio University, Athens and Department of Astronomy, University of Maryland, College Park The Yarkovsky effect describes a small but significant force that affects the orbital motion of meteoroids and asteroids smaller than 30 − 40 kilometers in diameter. It is caused by sunlight; when these bodies heat up in the Sun, they eventually re-radiate the energy away in the thermal waveband, which in turn creates a tiny thrust. This recoil acceleration is much weaker than solar and planetary gravitational forces, but it can produce measurable orbital changes over decades and substantial orbital effects over millions to billions of years. The same physical phenomenon also creates a thermal torque that, complemented by a torque produced by scattered sunlight, can modify the rotation rates and obliquities of small bodies as well. This rotational variant has been coined the Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) effect. During the past decade or so, the Yarkovsky and YORP effects have been used to explore and potentially resolve a number of unsolved mysteries in planetary science dealing with small bodies. Here we review the main results to date, and preview the goals for future work. 1. INTRODUCTION erature through the works of Vladimir V. Radzievskii and his collaborators (Radzievskii, 1952b). While Radzievskii Interesting problems in science usually have a long and was also the first to consider the effects of systematic pho- complex history.
    [Show full text]
  • Binary Asteroids in the Near-Earth Synchronous and Asynchronous to the Satellites Population As Well
    Asteroid Systems: Binaries, Triples, and Pairs Jean-Luc Margot University of California, Los Angeles Petr Pravec Astronomical Institute of the Czech Republic Academy of Sciences Patrick Taylor Arecibo Observatory Benoˆıt Carry Institut de Mecanique´ Celeste´ et de Calcul des Eph´ em´ erides´ Seth Jacobson Coteˆ d’Azur Observatory In the past decade, the number of known binary near-Earth asteroids has more than quadrupled and the number of known large main belt asteroids with satellites has doubled. Half a dozen triple asteroids have been discovered, and the previously unrecognized populations of asteroid pairs and small main belt binaries have been identified. The current observational evidence confirms that small (.20 km) binaries form by rotational fission and establishes that the YORP effect powers the spin-up process. A unifying paradigm based on rotational fission and post-fission dynamics can explain the formation of small binaries, triples, and pairs. Large(&20 km) binaries with small satellites are most likely created during large collisions. 1. INTRODUCTION composition and internal structure of minor plan- ets. Binary systems offer opportunities to mea- 1.1. Motivation sure thermal and mechanical properties, which are generally poorly known. Multiple-asteroid systems are important be- The binary and triple systems within near- cause they represent a sizable fraction of the aster- Earth asteroids (NEAs), main belt asteroids oid population and because they enable investiga- (MBAs), and trans-Neptunian objects (TNOs) ex- tions of a number of properties and processes that hibit a variety of formation mechanisms (Merline are often difficult to probe by other means. The et al. 2002c; Noll et al.
    [Show full text]
  • Techniques for Asteroid Spectrocopy Marcel Popescu
    Techniques for asteroid spectrocopy Marcel Popescu To cite this version: Marcel Popescu. Techniques for asteroid spectrocopy. Earth and Planetary Astrophysics [astro- ph.EP]. Observatoire de Paris; Universitatea Politehnica din Bucuresti, Facultatea de Ştiinţe Aplicate, 2012. English. tel-00785991 HAL Id: tel-00785991 https://tel.archives-ouvertes.fr/tel-00785991 Submitted on 7 Feb 2013 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. OBSERVATOIRE DE PARIS ÉCOLE DOCTORALE D’ASTRONOMIE ET D’ASTROPHYSIQUE D’ÎLE-DE-FRANCE ∗ UNIVERSITATEA POLITHENICA BUCURE¸STI FACULTATEA DE ¸STIIN ¸TE APLICATE DOCTORAL THESIS by Marcel Popescu TECHNIQUES FOR ASTEROID SPECTROSCOPY Defended the 23 Octobre 2012 before the jury: Vasile IFTODE (Universitatea Polithenica Bucure¸sti) President Olivier GROUSSIN (Laboratoire d’Astrophysique de Marseille) Reviewer Petre POPESCU (Institutul Astronomic al Academiei Române) Reviewer Dan DUMITRA¸S (INFLPR, România) Reviewer Jean SOUCHAY (SYRTE - Observatoire de Paris) Examiner Mirel BIRLAN (IMCCE - Observatoire de Paris) Co-Advisor
    [Show full text]
  • NEAR EARTH ASTEROIDS (Neas) a CHRONOLOGY of MILESTONES 1800 - 2200
    INTERNATIONAL ASTRONOMICAL UNION UNION ASTRONOMIQUE INTERNATIONALE NEAR EARTH ASTEROIDS (NEAs) A CHRONOLOGY OF MILESTONES 1800 - 2200 8 July 2013 – version 41.0 on-line: www.iau.org/public/nea/ (completeness not pretended) INTRODUCTION Asteroids, or minor planets, are small and often irregularly shaped celestial bodies. The known majority of them orbit the Sun in the so-called main asteroid belt, between the orbits of the planets Mars and Jupiter. However, due to gravitational perturbations caused by planets as well as non- gravitational perturbations, a continuous migration brings main-belt asteroids closer to Sun, thus crossing the orbits of Mars, Earth, Venus and Mercury. An asteroid is coined a Near Earth Asteroid (NEA) when its trajectory brings it within 1.3 AU [Astronomical Unit; for units, see below in section Glossary and Units] from the Sun and hence within 0.3 AU of the Earth's orbit. The largest known NEA is 1036 Ganymed (1924 TD, H = 9.45 mag, D = 31.7 km, Po = 4.34 yr). A NEA is said to be a Potentially Hazardous Asteroid (PHA) when its orbit comes to within 0.05 AU (= 19.5 LD [Lunar Distance] = 7.5 million km) of the Earth's orbit, the so-called Earth Minimum Orbit Intersection Distance (MOID), and has an absolute magnitude H < 22 mag (i.e., its diameter D > 140 m). The largest known PHA is 4179 Toutatis (1989 AC, H = 15.3 mag, D = 4.6×2.4×1.9 km, Po = 4.03 yr). As of 3 July 2013: - 903 NEAs (NEOWISE in the IR, 1 February 2011: 911) are known with D > 1000 m (H < 17.75 mag), i.e., 93 ± 4 % of an estimated population of 966 ± 45 NEAs (NEOWISE in the IR, 1 February 2011: 981 ± 19) (see: http://targetneo.jhuapl.edu/pdfs/sessions/TargetNEO-Session2-Harris.pdf, http://adsabs.harvard.edu/abs/2011ApJ...743..156M), including 160 PHAs.
    [Show full text]
  • Tidal Interactions in Binary Asteroid Systems
    TIDAL INTERACTIONS IN BINARY ASTEROID SYSTEMS A Dissertation Presented to the Faculty of the Graduate School of Cornell University in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy by Patrick Alan Taylor May 2009 c 2009 Patrick Alan Taylor ALL RIGHTS RESERVED TIDAL INTERACTIONS IN BINARY ASTEROID SYSTEMS Patrick Alan Taylor, Ph.D. Cornell University 2009 Tidal evolution in binary asteroid systems is examined with the dynamics extended to systems with close orbits within 5 radii of the primary component, non-negligibly eccentric mutual orbits, and a non-spherical primary component. The use of tidal evo- lution to determine the material properties of asteroids in terms of the product of the rigidity (shear modulus) and specific tidal dissipation function shows binary systems in the main belt with 100-km scale primary components are consistent with monolithic or fractured rock. Near-Earth binaries must either be much weaker mechanically than their main belt cousins, as one would expect for heavily fractured or rubble pile bodies, or have been formed in the main belt prior to injection to the near-Earth region. The most important factor in determining material properties of an asteroid in this manner is un- certainty in the age of the binary. The formation of contact binary systems where the two components are in physical contact and rotate as a single body is shown to be caused by the lack of a valid, stable, fully despun, double synchronous mutual orbit. Whether this lack of a tidal end state is caused during the formation process, with non-spherical components, or through the reduction of the angular momentum of the system via a spin-down mechanism, contact binaries are preferentially produced with components of similar size as is observed by radar.
    [Show full text]
  • Binary Minor Planets
    ANRV273-EA34-03 ARI 17 April 2006 23:17 Binary Minor Planets Derek C. Richardson and Kevin J. Walsh Department of Astronomy, University of Maryland, College Park, Maryland 20740-2421; email: [email protected], [email protected] Annu. Rev. Earth Planet. Sci. Key Words 2006. 34:47–81 First published online as a asteroids, comets, evolution, origin, satellites Review in Advance on October 31, 2005 Abstract The Annual Review of A review of observations and theories regarding binary asteroids and binary trans- Earth and Planetary Science Neptunian objects [collectively, binary minor planets (BMPs)] is presented. To date, is online at earth.annualreviews.org these objects have been discovered using a combination of direct imaging, lightcurve analysis, and radar. They are found throughout the Solar System, and present a chal- doi: 10.1146/ annurev.earth.32.101802.120208 lenge for theorists modeling their formation in the context of Solar System evolution. The most promising models invoke rotational disruption for the smallest, shortest- Copyright c 2006 by Annual Reviews. All rights lived objects (the asteroids nearest to Earth), consistent with the observed fast rotation reserved of these bodies; impacts for the larger, longer-lived asteroids in the main belt, con- 0084-6597/06/0530- sistent with the range of size ratios of their components and slower rotation rates; 0047$20.00 and mutual capture for the distant, icy, trans-Neptunian objects, consistent with their large component separations and near-equal sizes. Numerical simulations have suc- cessfully reproduced key features of the binaries in the first two categories; the third remains to be investigated in detail.
    [Show full text]
  • An Introduction to Near-Earth Objects
    AN INTRODUCTION TO NEAR-EARTH OBJECTS An Introduction to Near-Earth Objects Andrew S. Rivkin n 13 April 2029, an object the size of the APL campus (≈300 m across) will make its closest approach to Earth. At the beginning of January 2029, the object will be a dot visible only in large telescopes that know exactly where to point, 250,000 times too faint to be seen even by the sharpest-eyed person. In early February it will reach its aphelion and begin its return toward the Sun. The Earth, closer to the Sun and moving faster, will overtake the object: already the Earth and this asteroid will have closed the gap between them by nearly 40% since New Year’s Day, and the asteroid will have brightened by a factor of roughly 3. At the end of March, the incoming asteroid will have brightened by a factor of 100 since January. The next factor of 100 will take only 2 weeks. As clocks switch over on the East Coast to 13 April, a Friday, the Moon will briefly no longer be Oour nearest neighbor. As the morning rush hour winds down in the east, sharp-eyed people in dark sites on the other side of the globe will be able to discern the visitor. It will continue to brighten, moving north and west at tens of degrees per hour, reaching a peak brightness comparable to stars in the Big Dipper. Then the geometry between the Sun, Earth, and asteroid will have changed so the asteroid will first become gib- bous, then quarter phase.
    [Show full text]
  • Mineralogy and Surface Composition of Asteroids Vishnu Reddy Planetary Science Institute
    Mineralogy and Surface Composition of Asteroids Vishnu Reddy Planetary Science Institute Tasha L. Dunn Colby College Cristina A. Thomas NASA Goddard Spaceflight Center Nicholas A. Moskovitz Lowell Observatory Thomas H. Burbine Mount Holyoke College Methods to constrain the surface mineralogy of asteroids have seen considerable development during the last decade with advancement in laboratory spectral calibrations and validation of our interpretive methodologies by spacecraft rendezvous missions. This has enabled the accurate identification of several meteorite parent bodies in the main asteroid belt and helped constrain the mineral chemistries and abundances in ordinary chondrites and basaltic achondrites. With better quantification of spectral effects due to temperature, phase angle, and grain size, systematic discrepancies due to non- compositional factors can now be virtually eliminated for mafic silicate-bearing asteroids. Interpretation of spectrally featureless asteroids remains a challenge. This paper presents a review of all mineralogical interpretive tools currently in use and outlines procedures for their application. 1. INTRODUCTION Physical characterization of small bodies through the use of reflectance spectroscopy provides insight into the diversity of chemical compositions in the Solar System and enables meteorites in our terrestrial collections to be linked to specific parent bodies in space. Since the publication of Asteroids III there have been numerous advances in the mineralogical characterization of asteroid surfaces using visible/near- infrared (VIS/NIR) and mid-IR spectra. One of the most significant developments in ground-based characterization of small bodies over the last decade is the commissioning of the SpeX instrument in the NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawai’i. The ideal spectral resolution (~few hundred), wavelength range (0.8 –5 !m), and high altitude of Mauna Kea have facilitated the mineralogical characterization of asteroids down to a visual magnitude of 19.
    [Show full text]
  • Near-Earth Asteroid Surface Roughness Depends on Compositional Class ∗ Lance A.M
    ARTICLE IN PRESS YICAR:8714 JID:YICAR AID:8714 /FLA [m5G; v 1.65; Prn:8/10/2008; 15:52] P.1 (1-11) Icarus ••• (••••) •••–••• Contents lists available at ScienceDirect Icarus www.elsevier.com/locate/icarus Near-Earth asteroid surface roughness depends on compositional class ∗ Lance A.M. Benner a, ,StevenJ.Ostroa, Christopher Magri b, Michael C. Nolan c, Ellen S. Howell c, Jon D. Giorgini a, Raymond F. Jurgens a, Jean-Luc Margot d, Patrick A. Taylor d, Michael W. Busch e, Michael K. Shepard f a Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, 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 Department of Astronomy, Cornell University, Ithaca, NY 14853, USA e Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA f Department of Geography and Geosciences, Bloomsburg University, Bloomsburg, PA 17815, USA article info abstract Article history: Radar observations of 214 near-Earth asteroids (NEAs) reveal a very strong correlation of circular Received 21 February 2008 polarization ratio with visible–infrared taxonomic class, establishing distinct differences in the centimeter- Revised 18 June 2008 to-several-decimeter structural complexity of objects in different spectral classes. The correlation may be due to the intrinsic mechanical properties of different mineralogical assemblages but also may reflect very different formation ages and collisional histories. The highest ratios are measured for groups Keywords: Near-Earth objects associated with achondritic igneous rocky meteorites: the E class, whose parent body may be 3103 Asteroids Eger, and the V class, derived from the mainbelt asteroid (and Dawn mission target) 4 Vesta.
    [Show full text]