Large Primitive Asteroids, Europa-Like and Ceres-Like Groups (Groups 3 and 4)
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Dynamical Evolution of the Cybele Asteroids
MNRAS 451, 244–256 (2015) doi:10.1093/mnras/stv997 Dynamical evolution of the Cybele asteroids Downloaded from https://academic.oup.com/mnras/article-abstract/451/1/244/1381346 by Universidade Estadual Paulista J�lio de Mesquita Filho user on 22 April 2019 V. Carruba,1‹ D. Nesvorny,´ 2 S. Aljbaae1 andM.E.Huaman1 1UNESP, Univ. Estadual Paulista, Grupo de dinamicaˆ Orbital e Planetologia, 12516-410 Guaratingueta,´ SP, Brazil 2Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA Accepted 2015 May 1. Received 2015 May 1; in original form 2015 April 1 ABSTRACT The Cybele region, located between the 2J:-1A and 5J:-3A mean-motion resonances, is ad- jacent and exterior to the asteroid main belt. An increasing density of three-body resonances makes the region between the Cybele and Hilda populations dynamically unstable, so that the Cybele zone could be considered the last outpost of an extended main belt. The presence of binary asteroids with large primaries and small secondaries suggested that asteroid families should be found in this region, but only relatively recently the first dynamical groups were identified in this area. Among these, the Sylvia group has been proposed to be one of the oldest families in the extended main belt. In this work we identify families in the Cybele region in the context of the local dynamics and non-gravitational forces such as the Yarkovsky and stochastic Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effects. We confirm the detec- tion of the new Helga group at 3.65 au, which could extend the outer boundary of the Cybele region up to the 5J:-3A mean-motion resonance. -
Occultation Newsletter Volume 8, Number 4
Volume 12, Number 1 January 2005 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Article Page The Largest Members Of Our Solar System – 2005 . 4 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . .11 IOTA European Section (IOTA/ES) . .11 IOTA on the World Wide Web. Back Cover ON THE COVER: Steve Preston posted a prediction for the occultation of a 10.8-magnitude star in Orion, about 3° from Betelgeuse, by the asteroid (238) Hypatia, which had an expected diameter of 148 km. The predicted path passed over the San Francisco Bay area, and that turned out to be quite accurate, with only a small shift towards the north, enough to leave Richard Nolthenius, observing visually from the coast northwest of Santa Cruz, to have a miss. But farther north, three other observers video recorded the occultation from their homes, and they were fortuitously located to define three well- spaced chords across the asteroid to accurately measure its shape and location relative to the star, as shown in the figure. The dashed lines show the axes of the fitted ellipse, produced by Dave Herald’s WinOccult program. This demonstrates the good results that can be obtained by a few dedicated observers with a relatively faint star; a bright star and/or many observers are not always necessary to obtain solid useful observations. – David Dunham Publication Date for this issue: July 2005 Please note: The date shown on the cover is for subscription purposes only and does not reflect the actual publication date. -
University of Groningen Asteroid Thermophysical Modeling Delbo
University of Groningen Asteroid thermophysical modeling Delbo, Marco; Mueller, Michael; Emery, Joshua P.; Rozitis, Ben; Capria, Maria Teresa Published in: Asteroids IV IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2015 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Delbo, M., Mueller, M., Emery, J. P., Rozitis, B., & Capria, M. T. (2015). Asteroid thermophysical modeling. In P. Michel, F. E. DeMeo, & W. F. Botke (Eds.), Asteroids IV (pp. 107-128). tUSCON: University of Arizona Press. Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 13-11-2019 Asteroid thermophysical modeling Marco Delbo Laboratoire Lagrange, UNS-CNRS, Observatoire de la Coteˆ d’Azur Michael Mueller SRON Netherlands Institute for Space Research Joshua P. Emery Dept. of Earth and Planetary Sciences - University of Tennessee Ben Rozitis Dept. -
IRTF Spectra for 17 Asteroids from the C and X Complexes: a Discussion of Continuum Slopes and Their Relationships to C Chondrites and Phyllosilicates ⇑ Daniel R
Icarus 212 (2011) 682–696 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus IRTF spectra for 17 asteroids from the C and X complexes: A discussion of continuum slopes and their relationships to C chondrites and phyllosilicates ⇑ Daniel R. Ostrowski a, Claud H.S. Lacy a,b, Katherine M. Gietzen a, Derek W.G. Sears a,c, a Arkansas Center for Space and Planetary Sciences, University of Arkansas, Fayetteville, AR 72701, United States b Department of Physics, University of Arkansas, Fayetteville, AR 72701, United States c Department of Chemistry and Biochemistry, University of Arkansas, Fayetteville, AR 72701, United States article info abstract Article history: In order to gain further insight into their surface compositions and relationships with meteorites, we Received 23 April 2009 have obtained spectra for 17 C and X complex asteroids using NASA’s Infrared Telescope Facility and SpeX Revised 20 January 2011 infrared spectrometer. We augment these spectra with data in the visible region taken from the on-line Accepted 25 January 2011 databases. Only one of the 17 asteroids showed the three features usually associated with water, the UV Available online 1 February 2011 slope, a 0.7 lm feature and a 3 lm feature, while five show no evidence for water and 11 had one or two of these features. According to DeMeo et al. (2009), whose asteroid classification scheme we use here, 88% Keywords: of the variance in asteroid spectra is explained by continuum slope so that asteroids can also be charac- Asteroids, composition terized by the slopes of their continua. -
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. -
2005 Astronomy Magazine Index
2005 Astronomy Magazine Index Subject index flyby of Titan, 2:72–77 Einstein, Albert, 2:30–53 Cassiopeia (constellation), 11:20 See also relativity, theory of Numbers Cassiopeia A (supernova), stellar handwritten manuscript found, 3C 58 (star remnant), pulsar in, 3:24 remains inside, 9:22 12:26 3-inch telescopes, 12:84–89 Cat's Eye Nebula, dying star in, 1:24 Einstein rings, 11:27 87 Sylvia (asteroid), two moons of, Celestron's ExploraScope telescope, Elysium Planitia (on Mars), 5:30 12:33 2:92–94 Enceladus (Saturn's moon), 11:32 2003 UB313, 10:27, 11:68–69 Cepheid luminosities, 1:72 atmosphere of water vapor, 6:22 2004, review of, 1:31–40 Chasma Boreale (on Mars), 7:28 Cassini flyby, 7:62–65, 10:32 25143 (asteroid), 11:27 chonrites, and gamma-ray bursts, 5:30 Eros (asteroid), 11:28 coins, celestial images on, 3:72–73 Eso Chasma (on Mars), 7:28 color filters, 6:67 Espenak, Fred, 2:86–89 A Comet Hale-Bopp, 7:76–79 extrasolar comets, 9:30 Aeolis (on Mars), 3:28 comets extrasolar planets Alba Patera (Martian volcano), 2:28 from beyond solar system, 12:82 first image of, 4:20, 8:26 Aldrin, Buzz, 5:40–45 dust trails of, 12:72–73 first light from, who captured, 7:30 Altair (star), 9:20 evolution of, 9:46–51 newly discovered low-mass planets, Amalthea (Jupiter's moon), 9:28 extrasolar, 9:30 1:68–71 amateur telescopes. See telescopes, Conselice, Christopher, 1:20 smallest, 9:26 amateur constellations whether have diamond layers, 5:26 Andromeda Galaxy (M31), 10:84–89 See also names of specific extraterrestrial life, 4:28–34 disk of stars surrounding, 7:28 constellations eyepieces, telescope. -
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. -
Discovery of the Triple Asteroidal System 87 Sylvia
UC Berkeley UC Berkeley Previously Published Works Title Discovery of the triple asteroidal system 87 Sylvia Permalink https://escholarship.org/uc/item/7nb376hk Journal Nature, 436(7052) ISSN 0028-0836 Authors Marchis, F Descamps, P Hestroffer, D et al. Publication Date 2005-08-01 Peer reviewed eScholarship.org Powered by the California Digital Library University of California 1 Discovery of the Triple Asteroidal System (87) Sylvia Franck Marchis*, Pascal Descamps†, Daniel Hestroffer†, Jerome Berthier† *Department of Astronomy, 601 Campbell Hall, Berkeley CA 94720, USA † Institut De Mécanique Céleste et Calculs D’Éphémérides, Observatoire de Paris, 77 Avenue Denfert-Rochereau, F-75014 Paris, France ‘These authors contributed equally to this work’ These observations are based on data collected at the European Southern Observatory, Chile (73.C-0062 and 74.C-0052). After decades of speculation1, the existence of binary asteroids is now observationally confirmed2,3 and several have been discovered in all minor planet populations4. We report here the unambiguous detection of a triple asteroid system in the main-belt, composed of a 280-km primary (87 Sylvia) and two small moonlets orbiting at 710 and 1360 km. The excellent orbital coverage provided by ~2 months of observations allowed us to estimate separately their orbital elements and refine the shape of the primary. Both orbits are equatorial, circular, and prograde suggesting a common origin. Using Kepler’s third law on both orbits, the mass and density of the primary asteroid are consistent. 87 Sylvia appears to have a rubble-pile structure with a porosity of 25-60%. This triple system was most likely formed through a disruptive collision of a parent asteroid. -
(50278) 2000Cz12
A&A 455, L29–L31 (2006) Astronomy DOI: 10.1051/0004-6361:20065760 & c ESO 2006 Astrophysics Letter to the Editor New mass determination of (15) Eunomia based on a very close encounter with (50278) 2000CZ12 A. Vitagliano1 andR.M.Stoss2,3 1 Dipartimento di Chimica, Università di Napoli Federico II, Complesso Universitario di Monte S. Angelo, via Cintia, 80126 Napoli, Italy e-mail: [email protected] 2 Observatorio Astronómico de Mallorca, Camí de l’Observatori, 07144 Costitx, Mallorca, Spain 3 Astronomisches Rechen-Institut, Mönchhofstr. 12-14, 69120 Heidelberg, Germany Received 5 June 2006 / Accepted 22 June 2006 ABSTRACT Aims. The possibility of determining the mass of large asteroids (other than Ceres, Pallas, and Vesta) from recent close encounters with smaller bodies has been investigated, and a new and more accurate determination of the mass of the asteroid (15) Eunomia is presented. Methods. The circumstances of the close approaches between large asteroids and the ca. 129 000 numbered ones were found by a numerical integration over the past 20 years. The cases for which an appreciable perturbation could be expected were investigated by fitting the mass of the perturbing body to the available observations. Results. A very close approach took place on March 4, 2002, between Eunomia and (50278) 2000CZ12, at a nominal distance of 55 200 km. The resulting perturbation in the mean motion of the smaller body was substantially larger than for the other detected events, amounting to ca. 0.9 arcsecs/y. The orbital elements of (50278) 2000CZ12 were fitted together with the mass of Eunomia 19 −11 on 106 of 110 observations spanning 1950 to 2006, resulting in a mass of 3.25 × 10 kg (1.64 × 10 MSun) with a formal 1σ relative uncertainty of 3.7%. -
The Orbit and Size of (87) Sylvia¬タルs Romulus from the 2015 Apparition
Icarus 276 (2016) 107–115 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The orbit and size of (87) Sylvia’s Romulus from the 2015 apparition ∗ Jack D. Drummond , Odell R. Reynolds, Miles D. Buckman Starfire Optical Range, Directed Energy Directorate, Air Force Research Laboratory, Kirtland AFB, NM 87117-5771, USA a r t i c l e i n f o a b s t r a c t Article history: Using the US Air Force’s Starfire Optical Range 3.5 meter telescope with adaptive optics and a laser Received 11 December 2015 guidestar, we obtained 68 images of asteroid (87) Sylvia and its satellite Romulus over 6 nights in March Revised 23 March 2016 and May of 2015. Adding an additional 3 images from earlier observations on one night in November Accepted 20 April 2016 2012, we are able to derive a circular (but not an eccentric) orbit for Romulus, leading to a density for Available online 3 May 2016 Sylvia of 1.37 ± 0.04 gm/cm 3. Extending the time base to 14 years by combining our data with previ- Keywords: ous observations from Keck, HST, and the VLT reported in the literature, we can fit for a new circular Satellites of asteroids orbit and change the density estimate slightly to 1.35 ± 0.04 gm/cm 3. By fitting a ratio of two Fourier Adaptive optics series to the measured magnitude difference between Sylvia (V = 12.5) and Romulus, which ranged from Image processing 4.1 to 5.0 in the J-band ( λ = 1 . -
Les Principaux Astres Du Système Solaire
seconde 2009-2010 Les principaux astres du système solaire NB : les corps qui suivent n'étaient pas tous connus des astronomes de l'Antiquité, donc les noms latins et grecs ne sont que des transcriptions modernes. Les planètes et planètes naines sont mises en gras. La distance au Soleil n'est que la moyenne (demi-grand axe) entre l'aphélie et la périhélie ; exemple avec l'orbite de Sedna qui passe en 12 000 ans de 76,057 à 935,451 UA (demi-grand axe : 505,754 UA). Étant donné qu'au printemps 2009 l'Union astronomique internationale dénombrait plus de 450 000 astéroïdes dans notre système, tous ne sont pas présents ci-dessous... Sources : IAU ; Names & discoverers ; Minor Planet Center (Smithsonian). Noms Distances Années de Noms Noms systématiques Symboles au Soleil Noms latins Noms grecs découverte français anglais selon l'IAU (en UA) - 0,000 - Soleil Sol Ήλιος Sun Sol I 0,387 - Mercure Mercvrivs Ερμής Mercury - 0,635 2004 2004 JG6 2004 JG6 Sol II 0,723 - Vénus Venvs Αφροδίτη Venus - 0,723 2002 2002 VE68 2002 VE68 163693 - 0,741 2003 Atira Atira - 0,818 2004 2004 FH 2004 FH 2100 - 0,832 1978 Ra-Shalom Ra-Shalom 2340 - 0,844 1976 Hathor Hathor 99942 - 0,922 2004 Apophis Άποφις Apophis 2062 - 0,967 1976 Aten Aten - 0,997 2003 2003 YN107 2003 YN107 3753 - 0,998 1986 Cruithne Cruithne Sol III 1,000 - Terre Tellvs/Terra Γη/Γαῖα Earth Earth I - - Lune Lvna Σελήνη Moon - 1,000 2002 2002 AA29 2002 AA29 54509 - 1,005 2000 YORP YORP 4581 - 1,022 1989 Asclépios Asclepius 4769 - 1,063 1989 Castalia Castalia 1620 - 1,245 1951 Géographos Geographos -
Orbits of Near-Earth Asteroid Triples 2001 Sn263 and 1994 Cc: Properties, Origin, and Evolution
The Astronomical Journal, 141:154 (15pp), 2011 May doi:10.1088/0004-6256/141/5/154 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ORBITS OF NEAR-EARTH ASTEROID TRIPLES 2001 SN263 AND 1994 CC: PROPERTIES, ORIGIN, AND EVOLUTION Julia Fang1, Jean-Luc Margot1,2, Marina Brozovic3, Michael C. Nolan4, Lance A. M. Benner3, and Patrick A. Taylor4 1 Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 2 Department of Earth and Space Sciences, University of California Los Angeles, Los Angeles, CA 90095, USA 3 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA 4 Arecibo Observatory, National Astronomy and Ionosphere Center, Arecibo, PR 00612, USA Received 2010 December 9; accepted 2011 February 28; published 2011 March 30 ABSTRACT Three-body model fits to Arecibo and Goldstone radar data reveal the nature of two near-Earth asteroid triples. The triple-asteroid system 2001 SN263 is characterized by a primary of ∼1013 kg, an inner satellite ∼1% as massive orbiting at ∼3 primary radii in ∼0.7 days, and an outer satellite ∼2.5% as massive orbiting at ∼13 primary radii in ∼6.2 days. 1994 CC is a smaller system with a primary of mass ∼2.6 ×1011 kg and two satellites ∼2% and 1% as massive orbiting at distances of ∼5.5 and ∼19.5 primary radii. Their orbital periods are ∼1.2 and ∼8.4 days. Examination of resonant arguments shows that the satellites are not currently in a mean-motion resonance. Precession of the apses and nodes are detected in both systems (2001 SN263 inner body: d/dt ∼ 1.1 deg day−1; 1994 CC inner body: d/dt ∼−0.2 deg day−1), which is in agreement with analytical predictions of the secular evolution due to mutually interacting orbits and primary oblateness.