DOCSLIB.ORG

Lunar and Planetary Science XXXII (2001) 1611.Pdf

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Lunar and Planetary Science XXXII (2001) 1611.Pdf Lunar and Planetary Science XXXII (2001) 1611.pdf ASTEROID BULK DENSITY: IMPLICATIONS FOR THE STRUCTURE OF ASTEROIDS. D. T. Britt1 and G. J. Consolmagno SJ2, 1Department of Geological Sciences, University of Tennessee, Knoxville, TN 37996, dbritt@utk.edu. 2Vatican Observatory, V-00120, Vatican City State, gjc@specola.va. Introduction: The numbers of asteroid bulk density teorite analogue microporosity from the bulk porosity of measurements have been rapidly increasing thanks to an asteroid provides a rough estimate of the asteroid’s spacecraft missions [1,2], observations of asteroid satel- large-scale macroporosity. An asteroids macroporosity lites [3,4], observations of asteroid mutual gravitational are the fractures, cracks, and voids that are large enough events [5,6,7], and radar observations. These data, along to effect its coherent strength. It is the estimate of with data on the grain densities of analogue meteorites macroporosity that can provide insight into the internal can provide significant insight on asteroid porosity and structure of an asteroid. Note that this estimate requires internal structure. Shown in Figure 1 are bulk density two assumptions: First that we know the asteroid’s me- measurements for 11 asteroids, two bulk density aver- teorite analog and, second, that the meteorites delivered ages for C and S type asteroids, and bulk density meas- to Earth are a representative sample of that material. urements for the small, asteroid-like Martian moons Both assumptions are open to debate for almost any of Phobos and Deimos. Also included for comparison are these asteroids so the estimates presented here should be the average grain densities of CI, CM, and CV carbona- viewed with healthy skepticism. ceous chondrite meteorites (shown as red labeled verti- Shown in Figure 2 are asteroidal estimated macropo- cal lines) and range of ordinary chondrite meteorite rosities for the measured asteroids. These data appear to grain densities (shown as a gray box). Note that the divide into three rough groups. The first group include definition of bulk density is the mass of an object di- the large asteroids 1 Ceres, 2 Pallas, and 4 Vesta. Their vided by its volume including the volume of its pore bulk densities are very close to the bulk densities of their spaces. Grain density is the mass of an object divided analogue meteorites, indicating essentially zero macro- by the volume occupied by the mineral grains, excluding porosity. These asteroids are probably strong, coherent the volume of its pore spaces. The difference between objects that have not been disrupted through solar sys- bulk and grain density provides insight into the porosity tem history. It is interesting that all the three asteroids of an object. with diameters > 500 km all fall in the zero macroporos- Discussion: Figure 1 shows the large range of as- ity group. teroid bulk densities that, in most cases, tend to be sub- The second group includes the S asteroids 433 Eros stantially below their most likely meteorite analogues, and 243 Ida as well as 762 Pulcova and 121 Hermione. indicating significant porosity. The bulk porosity of These asteroids have between 15 and 25% macroporos- these asteroids can be estimated by using the grain den- ity indicating that they have been extensively fractured. sity data of the analogue meteorites to constrain the Spacecraft images of both 433 Eros and 243 Ida show amount of pore space that would be required for a object numerous morphological indications of pervasive frac- of that composition and measured bulk density. For turing [8,4]. However, this fracturing was probably not example 433 Eros has a measured bulk density of 2.67 ± extensive enough to disrupt the object and asteroids with 0.03 g/cm3 and probably has an L-chondrite composition less than approximately 25% macroporosity probably which implies a grain density of 3.75 g/cm3 [8]. To have some measure of coherent strength. In terrestrial make the L-chondrite grain density consistent with the geology, well-sorted sedimentary rocks can have up to asteroidal bulk density would require a bulk porosity of 30% porosity and still be coherent. However, over 30% 28.8% [9]. Similarly, 253 Mathilde has a measured bulk porosity usually indicates loose rubble or soils (volcanic density of 1.3 ± 0.2 g/cm3 and a possible CM composi- scoria can have up to 90% porosity, but this is an tion that implies a grain density of 2.71 g/cm3 [2]. This unlikely analogue for most asteroids). gives a bulk porosity of 52%. The third group are those with greater than 30% Both these bulk porosity numbers seem high and are macroporosity. These objects are probably pervasively a bit misleading for assessing the structure of the aster- fractured and may have been disrupted and reassembled oid. We can take the analysis a step farther by recogniz- by mutual gravity, some of which have more empty space ing that most meteorites have some level of micron-scale than solid material. Asteroid 16 Psyche is likely the most microporosity (ordinary chondrites for instance average porous object observed so far. Its reflectance spectra about 10% microporosity, CM carbonaceous chondrites and radar albedo strongly indicate a metallic surface average about 12% microporosity) that does not seri- composition. Assuming a iron meteorite grain density 3 ously effect the meteorite’s cohesive strength. The im- of 7.4 g/cm , this would require a bulk porosity of 75%! plication is that microporosity would also not effect the Iron meteorites have essentially zero microporosity, so parent asteroid’s strength. Subtracting the average me- the bulk porosity would in this case likely equals the macroporosity suggesting a pervasively disrupted object Lunar and Planetary Science XXXII (2001) 1611.pdf ASTEROID BULK DENSITY D. T. Britt and G. J. Consolmagno SJ that has been loosely reassembled and held together by 314.10-127. [7] Hilton J. L. (1999) AJ, 177, 1077- mutual gravitation. 1086. [8] Veverka J. et al. (2000) Science, 289, 2088– References: [1] Yeomans D. K. et al. (2000) Sci- 2097. [9] Britt D. T. et al. (2001) This Volume. ence, 289, 2085–2088. [2] Veverka J. et al., (1997) Sci- ence, 278, 2109-2114. [3] Merline W. J. (1999) Nature, 401, 565-568. [4] Belton, M.J.S. et al., (1995) Nature 373, 785-788. [5] Viateau, B (2000) Ast. & Astrophy. 354, 725-731. [6] Standish E. M. et al. (1995) JPL IOM Figure 1: Asteroid and Meteorite Density 1E+22 y 1 Ceres (G) s 2 Pallas (B) 4 Vesta (V) 1E+20 16 Psyche (M) 45 Eugenia (C) 762 Pulcova (F) CM Grain Densit 121 Hermione (C) 1E+18 90 Antiope (C) Average C Average S Chondrite Grain Densitie y 253 Mathilde (C) n 243 Ida (S) CV Grain Density 1E+16 Mass in Kg (log scale) Phobos CI Grai 433 Eros (S) Ordinar Deimos 1E+14 0.511.522.533.54 Density (g/cm3) Figure 2: Estimated Macroporosity 1E+22 1 Ceres (G) 4 Vesta (V) 2 Pallas (B) 1E+20 16 Psyche (M) 762 Pulcova (F) 45 Eugenia (C) 121 Hermione (C) 90 Antiope (C) 1E+18 e Average S Average C 253 Mathilde (C) 243 Ida (S) 1E+16 Mass in Kg (log scale) 433 Eros (S) Phobos Rubble Piles? Coherent Objects? Deimos Transition Zon 1E+14 0% 10% 20% 30% 40% 50% 60% 70% 80% Macroporosity .
Load more
Loading...
Loading...

—— Preview end. ——

Recommended publications
  • Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations*
    Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations* F. Marchisa,g, J.E. Enriqueza, J. P. Emeryb, M. Muellerc, M. Baeka, J. Pollockd, M. Assafine, R. Vieira Martinsf, J. Berthierg, F. Vachierg, D. P. Cruikshankh, L. Limi, D. Reichartj, K. Ivarsenj, J. Haislipj, A. LaCluyzej 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 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, United States j. Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27514, U.S.A * Based in part on observations collected at the European Southern Observatory, Chile Programs Numbers 70.C-0543 and ID 72.C-0753 Corresponding author: Franck Marchis Carl Sagan Center SETI Institute 189 Bernardo Ave. Mountain View CA 94043 USA fmarchis@seti.org Abstract: We collected mid-IR spectra from 5.2 to 38 µm using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups.
    [Show full text]
  • SMALL BODIES: SHAPES of THINGS to COME 8:30 A.M
    40th Lunar and Planetary Science Conference (2009) sess404.pdf Wednesday, March 25, 2009 SMALL BODIES: SHAPES OF THINGS TO COME 8:30 a.m. Waterway Ballroom 6 Chairs: Al Conrad Debra Buczkowski 8:30 a.m. Conrad A. R. * Merline W. J. Drummond J. D. Carry B. Dumas C. Campbell R. D. Goodrich R. W. Chapman C. R. Tamblyn P. M. Recent Results from Imaging Asteroids with Adaptive Optics [#2414] We report results from recent high-angular-resolution observations of asteroids using adaptive optics (AO) on large telescopes. 8:45 a.m. Marchis F. * Descamps P. Durech J. Emery J. P. Harris A. W. Kaasalainen M. Berthier J. The Cybele Binary Asteroid 121 Hermione Revisited [#1336] The combination of adaptive optics, photometric and Spitzer mid-IR observations of the 121 Hermione binary asteroid system allowed us to confirm the bilobated nature of the primary derived a bulk density of 1.4 g/cc implying a rubble-pile interior. 9:00 a.m. Schmidt B. E. * Thomas P. C. Bauer J. M. Li J. -Y. Radcliffe S. C. McFadden L. A. Mutchler M. J. Parker J. Wm. Rivkin A. S. Russell C. T. Stern S. A. The 3D Figure and Surface of Pallas from HST [#2421] We present Pallas in three dimensions and surface maps. 9:15 a.m. Besse S. * Groussin O. Jorda L. Lamy P. Kaasalainen M. Gesquiere G. Remy E. OSIRIS Team 3-Dimensional Reconstruction of Asteroid 2867 Steins [#1545] The OSIRIS imaging experiment has imaged asteroid Steins. We have combined three methods to retrieve the shape: limbs, Point of Interest and light curves.
    [Show full text]
  • A Low Density of 0.8 G Cm-3 for the Trojan Binary Asteroid 617 Patroclus
    Publisher: NPG; Journal: Nature:Nature; Article Type: Physics letter DOI: 10.1038/nature04350 A low density of 0.8 g cm−3 for the Trojan binary asteroid 617 Patroclus Franck Marchis1, Daniel Hestroffer2, Pascal Descamps2, Jérôme Berthier2, Antonin H. Bouchez3, Randall D. Campbell3, Jason C. Y. Chin3, Marcos A. van Dam3, Scott K. Hartman3, Erik M. Johansson3, Robert E. Lafon3, David Le Mignant3, Imke de Pater1, Paul J. Stomski3, Doug M. Summers3, Frederic Vachier2, Peter L. Wizinovich3 & Michael H. Wong1 1Department of Astronomy, University of California, 601 Campbell Hall, Berkeley, California 94720, USA. 2Institut de Mécanique Céleste et de Calculs des Éphémérides, UMR CNRS 8028, Observatoire de Paris, 77 Avenue Denfert-Rochereau, F-75014 Paris, France. 3W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, Hawaii 96743, USA. The Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter–Sun system (leading and following Jupiter by 60°). The asteroid 617 Patroclus is the only known binary Trojan1. The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680 km, move around the system’s centre of mass, describing a roughly circular orbit. Using this orbital information, combined with thermal measurements to estimate +0.2 −3 the size of the components, we derive a very low density of 0.8 −0.1 g cm . The components of 617 Patroclus are therefore very porous or composed mostly of water ice, suggesting that they could have been formed in the outer part of the Solar System2.
    [Show full text]
  • Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
    Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: sonia.fornasier@obspm.fr; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: sonia.fornasier@obspm.fr 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals.
    [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 Handbook of the British Astronomical Association
    THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2012 Saturn’s great white spot of 2011 2011 October ISSN 0068-130-X CONTENTS CALENDAR 2012 . 2 PREFACE. 3 HIGHLIGHTS FOR 2012. 4 SKY DIARY . .. 5 VISIBILITY OF PLANETS. 6 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S. 7-8 ECLIPSES . 9-15 TIME. 16-17 EARTH AND SUN. 18-20 MOON . 21 SUN’S SELENOGRAPHIC COLONGITUDE. 22 MOONRISE AND MOONSET . 23-27 LUNAR OCCULTATIONS . 28-34 GRAZING LUNAR OCCULTATIONS. 35-36 PLANETS – EXPLANATION OF TABLES. 37 APPEARANCE OF PLANETS. 38 MERCURY. 39-40 VENUS. 41 MARS. 42-43 ASTEROIDS AND DWARF PLANETS. 44-60 JUPITER . 61-64 SATELLITES OF JUPITER . 65-79 SATURN. 80-83 SATELLITES OF SATURN . 84-87 URANUS. 88 NEPTUNE. 89 COMETS. 90-96 METEOR DIARY . 97-99 VARIABLE STARS . 100-105 Algol; λ Tauri; RZ Cassiopeiae; Mira Stars; eta Geminorum EPHEMERIDES OF DOUBLE STARS . 106-107 BRIGHT STARS . 108 ACTIVE GALAXIES . 109 INTERNET RESOURCES. 110-111 GREEK ALPHABET. 111 ERRATA . 112 Front Cover: Saturn’s great white spot of 2011: Image taken on 2011 March 21 00:10 UT by Damian Peach using a 356mm reflector and PGR Flea3 camera from Selsey, UK. Processed with Registax and Photoshop. British Astronomical Association HANDBOOK FOR 2012 NINETY-FIRST YEAR OF PUBLICATION BURLINGTON HOUSE, PICCADILLY, LONDON, W1J 0DU Telephone 020 7734 4145 2 CALENDAR 2012 January February March April May June July August September October November December Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day of of of of of of of of of of of of of of of of of of of of of of of of of Month Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year 1 Sun.
    [Show full text]
  • Asteroids Do Have Satellites
    Asteroids Do Have Satellites William J. Merline Southwest Research Institute (Boulder) Stuart J. Weidenschilling Planetary Science Institute Daniel D. Durda Southwest Research Institute (Boulder) Jean-Luc Margot California Institute of Technology Petr Pravec Astronomical Institute AS CR, Ondrejoˇ v, Czech Republic and Alex D. Storrs Towson University After years of speculation, satellites of asteroids have now been shown definitively to exist. Asteroid satellites are important in at least two ways: (1) they are a natural laboratory in which to study collisions, a ubiquitous and critically important process in the formation and evolution of the asteroids and in shaping much of the solar system, and (2) their presence allows to us to determine the density of the primary asteroid, something which otherwise (except for certain large asteroids that may have measurable gravitational influence on, e.g., Mars) would require a spacecraft flyby, orbital mission, or sample return. Satellites or binaries have now been detected in a variety of dynamical populations, including near- Earth, Main Belt, outer Main-Belt, Trojan, and trans-Neptunian. Detection of these new systems has been the result of improved observational techniques, including adaptive op- tics on large telescopes, radar, direct imaging, advanced lightcurve analysis, and spacecraft imaging. Systematics and differences among the observed systems give clues to the for- mation mechanisms. We describe several processes that may result in binary systems, all of which involve collisions of one type or another, either physical or gravitational. Several mechanisms will likely be required to explain the observations. 1 1 INTRODUCTION 1.1 Overview Discovery and study of small satellites of asteroids or double asteroids can yield valuable infor- mation about the intrinsic properties of asteroids themselves and about their history and evolution.
    [Show full text]
  • Binary Asteroid Lightcurves
    BINARY ASTEROID LIGHTCURVES Asteroid Type Per1 Amp1 Per2 Amp2 Perorb Ds/Dp a/Dp Reference 22 Kalliope B 4.1483 0.53 B a Descamps, 08 B a 86.2896 Marchis, 08 B a 4.148 86.16 Marchis, 11w 41∗ Daphne B 5.988 0.45 B s 26.4 Conrad, 08 B s 38. Conrad, 08 B s 5.987981 27.289 2.46 Carry, 18 45 Eugenia M 5.699 0.30 B a 113. Merline, 99 B a Marchis, 06 M a Marchis, 07 M a Marchis, 08 B a 5.6991 114.38 Marchis, 11w 87 Sylvia M 5.184 0.50 M a 5.184 87.5904 Marchis, 05 M a 5.1836 87.59 Marchis, 11w 90∗ Antiope B 16.509 0.88 B f 16. Merline, 00 B f 16.509 0.73 16.509 0.73 16.509 Descamps, 05 B f 16.5045 0.86 16.5045 0.86 16.5045 Behrend, 07w B f 16.505046 16.505046 Bartczak, 14 93 Minerva M 5.982 0.20 M a 5.982 0.20 57.79 Marchis, 11 107∗ Camilla M 4.844 0.53 B a Marchis, 08 B a 4.8439 89.04 Marchis, 11w M a 1.550 Marsset, 16 M s 89.096 4.91 Pajuelo, 18 113 Amalthea B? 9.950 0.22 ? u Maley, 17 121 Hermione B 5.55128 0.62 B a Merline, 02 B a Marchis, 04 B a Marchis, 05 B a 5.55 61.97 Marchis, 11w 130 Elektra M 5.225 0.58 B a 5.22 126.2 Marchis, 08 M a Yang, 14 216 Kleopatra M 5.385 1.22 M a 5.38 Marchis, 08 243 Ida B 4.634 0.86 B a Belton, 94 279 Thule B? 23.896 0.10 B s 7.44 0.08 72.2 Sato, 15 283 Emma B 6.896 0.53 B a Merline, 03 B a 6.89 80.48 Marchis, 08 324 Bamberga B? 29.43 0.12 B s 29.458 0.06 71.0 Sato, 15 379 Huenna B 14.141 0.12 B a Margot, 03 B a 4.022 2102.
    [Show full text]
  • The Cybele Binary Asteroid 121 Hermione Revisited F
    40th Lunar and Planetary Science Conference (2009) 1336.pdf THE CYBELE BINARY ASTEROID 121 HERMIONE REVISITED F. Marchis1,2,3, P. Descamps3, J. Durech4, J.P Emery5, A.W. Harris6, M. Kaasalainen7, and J. Berthier3, 1SETI Institute, Carl Sagan Center, 515 N. Whisman Road, Mountain view CA 94043, USA, fmarchis@seti.org. 2UC-Berkeley, Dept of Astronomy, 601 Campbell Hall, Berkeley CA 94720, USA. 3Institut de Mécanique Céleste et de Calcul des Éphémérides, Observatoire de Paris, France, descamps@imcce.fr. 4Astronomical Institute, Charles University, Prague, Czech Republic 5University of Tennessee, Knoxville, USA. 6DLR, Berlin, Germany. 7Dept of Mathematics, University of Helsinki, Finland. Introduction: (121) Hermione is a Cybele group Satellite of Hermione: Additional observations of binary asteroid with a km-size moonlet discovered in the satellite were recorded using the Very Large Tele- 2002 [1]. The ~200-km primary was conjectured to be scope AO system in May 2006 and the Keck telescope bilobated [2] based on Adaptive Optics (AO) observa- in September 2008. The size of the satellite is re- tions. Because of the limited angular resolution of the estimated to a diameter of ~32 km. The orbit solution AO observations (~60 mas) its size and shape were was improved but does not vary significantly from that poorly constrained, impacting its bulk density estimate previously published [2]. The satellite orbits around which ranged between 0.8 and 2.0 g/cm3. From the the primary in 2.5632±0.0021 days describing a circu- determination of the orbital characteristics of Hermi- lar orbit (e<0.02) with a radius of 747±11 km.
    [Show full text]
  • Spectroscopy of B-Type Asteroids: Subgroups and Meteorite Analogs
    University of Central Florida STARS Faculty Bibliography 2010s Faculty Bibliography 1-1-2010 Spectroscopy of B-type asteroids: Subgroups and meteorite analogs Beth Ellen Clark Julie Ziffer David Nesvorny Humberto Campins University of Central Florida Andrew S. Rivkin See next page for additional authors Find similar works at: https://stars.library.ucf.edu/facultybib2010 University of Central Florida Libraries http://library.ucf.edu This Article is brought to you for free and open access by the Faculty Bibliography at STARS. It has been accepted for inclusion in Faculty Bibliography 2010s by an authorized administrator of STARS. For more information, please contact STARS@ucf.edu. Recommended Citation Clark, Beth Ellen; Ziffer, Julie; Nesvorny, David; Campins, Humberto; Rivkin, Andrew S.; Hiroi, Takahiro; Barucci, Maria Antonietta; Fulchignoni, Marcello; Binzel, Richard P.; Fornasier, Sonia; DeMeo, Francesca; Ockert-Bell, Maureen E.; Licandro, Javier; and Mothé-Diniz, Thais, "Spectroscopy of B-type asteroids: Subgroups and meteorite analogs" (2010). Faculty Bibliography 2010s. 48. https://stars.library.ucf.edu/facultybib2010/48 Authors Beth Ellen Clark, Julie Ziffer, David Nesvorny, Humberto Campins, Andrew S. Rivkin, Takahiro Hiroi, Maria Antonietta Barucci, Marcello Fulchignoni, Richard P. Binzel, Sonia Fornasier, Francesca DeMeo, Maureen E. Ockert-Bell, Javier Licandro, and Thais Mothé-Diniz This article is available at STARS: https://stars.library.ucf.edu/facultybib2010/48 JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, E06005, doi:10.1029/2009JE003478, 2010 Click Here for Full Article Spectroscopy of B‐type asteroids: Subgroups and meteorite analogs Beth Ellen Clark,1 Julie Ziffer,2 David Nesvorny,3 Humberto Campins,4 Andrew S. Rivkin,5 Takahiro Hiroi,6 Maria Antonietta Barucci,7 Marcello Fulchignoni,7 Richard P.
    [Show full text]
  • Updated on 1 September 2018
    20813 Aakashshah 12608 Aesop 17225 Alanschorn 266 Aline 31901 Amitscheer 30788 Angekauffmann 2341 Aoluta 23325 Arroyo 15838 Auclair 24649 Balaklava 26557 Aakritijain 446 Aeternitas 20341 Alanstack 8651 Alineraynal 39678 Ammannito 11911 Angel 19701 Aomori 33179 Arsenewenger 9117 Aude 16116 Balakrishnan 28698 Aakshi 132 Aethra 21330 Alanwhitman 214136 Alinghi 871 Amneris 28822 Angelabarker 3810 Aoraki 29995 Arshavsky 184535 Audouze 3749 Balam 28828 Aalamiharandi 1064 Aethusa 2500 Alascattalo 108140 Alir 2437 Amnestia 129151 Angelaboggs 4094 Aoshima 404 Arsinoe 4238 Audrey 27381 Balasingam 33181 Aalokpatwa 1142 Aetolia 19148 Alaska 14225 Alisahamilton 32062 Amolpunjabi 274137 Angelaglinos 3400 Aotearoa 7212 Artaxerxes 31677 Audreyglende 20821 Balasridhar 677 Aaltje 22993 Aferrari 200069 Alastor 2526 Alisary 1221 Amor 16132 Angelakim 9886 Aoyagi 113951 Artdavidsen 20004 Audrey-Lucienne 26634 Balasubramanian 2676 Aarhus 15467 Aflorsch 702 Alauda 27091 Alisonbick 58214 Amorim 30031 Angelakong 11258 Aoyama 44455 Artdula 14252 Audreymeyer 2242 Balaton 129100 Aaronammons 1187 Afra 5576 Albanese 7517 Alisondoane 8721 AMOS 22064 Angelalewis 18639 Aoyunzhiyuanzhe 1956 Artek 133007 Audreysimmons 9289 Balau 22656 Aaronburrows 1193 Africa 111468 Alba Regia 21558 Alisonliu 2948 Amosov 9428 Angelalouise 90022 Apache Point 11010 Artemieva 75564 Audubon 214081 Balavoine 25677 Aaronenten 6391 Africano 31468 Albastaki 16023 Alisonyee 198 Ampella 25402 Angelanorse 134130 Apaczai 105 Artemis 9908 Aue 114991 Balazs 11451 Aarongolden 3326 Agafonikov 10051 Albee
    [Show full text]
  • Simultaneous Spectroscopic and Photometric Observations of Binary Asteroids
    Simultaneous spectroscopic and photometric observations of binary asteroids Item Type Article; text Authors Polishook, D.; Brosch, N.; Prialnik, D.; Kaspi, S. Citation Polishook, D., Brosch, N., Prialnik, D., & Kaspi, S. (2009). Simultaneous spectroscopic and photometric observations of binary asteroids. Meteoritics & Planetary Science, 44(12), 1955-1966. DOI 10.1111/j.1945-5100.2009.tb02005.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 02/10/2021 17:33:49 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656659 Meteoritics & Planetary Science 44, Nr 12, 1955–1966 (2009) Abstract available online at http://meteoritics.org Simultaneous spectroscopic and photometric observations of binary asteroids D. POLISHOOK1, 2*, N. BROSCH2, D. PRIALNIK1, and S. KASPI2 1Department of Geophysics and Planetary Sciences, Tel-Aviv University, Tel-Aviv 69978, Israel 2The Wise Observatory and the Raymond and Beverly Sackler School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel *Corresponding author. E-mail: david@wise.tau.ac.il (Received 27 November 2008; revision accepted 30 August 2009) Abstract–We present results of visible wavelengths spectroscopic measurements (0.45 to 0.72 microns) of two binary asteroids, obtained with the 1-m telescope at the Wise Observatory on January 2008. The asteroids 90 Antiope and 1509 Esclangona were observed to search for spectroscopic variations correlated with their rotation while presenting different regions of their surface to the viewer. Simultaneous photometric observations were performed with the Wise Observatory’s 0.46 m telescope, to investigate the rotational phase behavior and possible eclipse events.
    [Show full text]