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Cambridge University Press 978-0-521-89935-2 - Patrick Moore’s Data Book of Astronomy Edited by Patrick Moore and Robin Rees Index More information Index 3C-273 in Virgo 360 Anderson, J. D. and W. B. Hubbard model Aristarchus 526 47 Tucani cluster 349 of Jupiter 183 Aristotle, 127, 288 Planet X and movements of Uranus and Armstrong, Neil 34 Abbott, Charles 13 Neptune 251 Arp 148 362 Abell 370 cluster of galaxies 361 Anderson, L. 248 Arp, Halton 366 Absolute magnitude, conversion to luminosity Andromeda 373 Arrhenius, Svante 122, 272 (table) 304 M31 361 and meteor crater 285 Achondrites 281 spiral 3, 338 Ashen light 109 Acidalia 137 spiral 338 explanations: Gruithuisen, Herschel 109 Active Galactic Nulcei (AGN) 358 spiral galaxy, distance 357 modern theory 109–110 Active galaxies 358 Andromedid meteor shower 273 Asher, D. 277 Adams, J. C. 224 Anglo-Australian Observatory 512 Assyrians data collector 526 calculations of the outer planets 235 Anglo-Australian telescope 306 Asterisms 370 Adams, W. S. 110, 132, 319 Angstrom, A. 9 Summer Triangle 372 Adel, A. 226 Angstrom, Anders 291 Asteroid 1036 Ganymed 171 Adhara, epsilon Canis Major, brightest EUV source 521 Angstrom unit 10 Asteroid 1200 Phaethon 163 Adrastea 189 Annular eclipses, British, list of 22 Asteroid 1566 Icarus 169 Aegospotamos, Greece 416BC 280 Ant nebula 351 Asteroid 1620 Geographos 171 Aerogel 268 Antarctica 364 Asteroid 2001QE24 157 Aerolites 280 meteorites in 280 Asteroid 2008 TC3, collision with 169 Ahnighito meteorite 281 Antares 319 Asteroid 2060 Chiron 177 Airglow 291 Antennae galaxies 358 Asteroid 21 Lutetia 167 Airy, G. B. movements of Uranus 235 Antlia 376 Asteroid 216 Kleopatra 167 Airy, Sir George 142, 179 Antoniardo, E. M. 203 Asteroid 24 Themis 167 Aitken, R. 315 map of Mercury 95 Asteroid 279 Thule 165 Akatsuki 112 AP Librae 360 Asteroid 31005, Phaethon 273 Al Sufi 355, 361 Apennines, lunar 28 Asteroid 3200 Phaethon 170 Alba Patera 136 Apex of the Sun’s Way 23 Asteroid 3735 Cruithne 168 Alban Hill meteorite, 634BC 280 Aphrodite Terra 114 Asteroid 3753, Cruithne 27 Albor Tholus 136 Apohele 168 Asteroid 4179 Toutatis 171 Alcyonides 209 Apollo 15 30 Asteroid 511 Davida 167 Aldebaran 303 Apollo basin Asteroid 5145 Pholus 177 Aldrin, Buzz 34 Apus 376 Asteroid 704 Interamnia 167 Al-Falavi 108 Aquarius 377 Asteroid 719 Albert 157 Alfven waves 17 EZ Aquarii 293 Asteroid 8335 Damocles 178 Algol 319 Aquila 380 Asteroid 87 Sylvia 173 Ali Ibn Ridwan 335 Ara 382 Asteroid 944 Hidalgo 177 Allen, D. A. 228 m Arae, 4 planets of 312 Asteroid 951 Gaspra 171 Al-Ma’mun 526 Arab astronomy, Baghdad school 526 Asteroid 99942 Apophis, close approach 168 Alpher, Bethe, Gamow theory 364 Arachnoids 119 belts (table) 172 Alpher, Ralph 363 Arago, F. 128 of other stars?, z leporis 178 Alphonsine tables of planetary motion 526 Arches cluster 355 Asteroid classes 168 Al-Sufi 526 Arcturus 303, 304 Apollos 169 Altjira (148780) 253 past and future 298 families (table) 164, 165 Alvarez, Luiz and Walter 81 Arecibo Observatory 358 Hermes 157 Amalthea 189 Arend–Roland comet 1957 270 hunting 162 craters on 189 Ares Valles 135, 140 impact theory of extinctions 122 features (table) 189 Argelander, F. W. 323 impacts 169 gossamer ring 189 Argo Navis divided up 367 Lutetia, past by Rosetta 268 surface of 189 Aricebo observatory 306 Centaurs 174 Ambartsumian, Viktor 348 Aricebo Radio Telescope 42, 349 Asteroids connected with comets 163 American unltaviolet satellites 521 Ariel, features (table) 232 outside the main belt 156 Anaxagoras 4, 288 Aries 384 with satellites (table) 175 and Democritus 354 g Arietis 315 Asteroids, 588 Achilles 174 and lunar eclipses 45 Aristarchus 4, 526 also classed as comets 163 560 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-89935-2 - Patrick Moore’s Data Book of Astronomy Edited by Patrick Moore and Robin Rees Index More information Index 561 Amor type (table) 172 Auroral noise 290 Bishop’s Ring 291 Centaurs (table) 177 ovals 289 Bjorgevskii, S. 361 classification of 164 Australia Radio Telescope 525 BL Lacertae objects 358 cometary 178 Black aurorae 290 Damocloids (table) 178 Baade, W. 169, 301, 305, 306, 357 Black drop 4, 108 diameters and absolute magnitudes (table) 168 Babcock 6 Black dwarf stars 303 encounters with (table) 171 Baby Boom galaxy 362 Black eye galaxy M64 362 first 100 main belt (table) 158–161 Baby Red Spot 182 Black hole at centre of Galaxy 307 first four (table) 157 Babylonian astronomy 526 formation 306 further out from Main Belt 174 Backwards galaxy NGC 4622 362 rotating 307 Geographos 42 Baily’s Beads 22 Black holes 306 identifications 157 Baldwin, Ralph 31 evaporating 307 influence of Jupiter 166 Ball, W. 203 isolated 307 Jupiter Trojans 174, 177 Barabaschev, N. 132 Black Saturday 22 largest 165 Barnard 2, P/177 264 Blanpain’s comet 265 Main Belt 156, 165 Barnard, E. E. 203 Blazars 358 Mars crossers 169 Barnard’s star 293, 297 Blaze star (T Coronae Borealis) 331 moving close to the Sun 169 Barnard’s star, reported planet 309 Blinking planetary nebula 351 names of 157 Bar-Nun, Akiva, analysis of Titan lakes 217 BL-Lacertae objects, nature 360 near Earth 1 Baroness de Podmaniczky 327 Blue Moons 25 near Earth class 168 Barr, J, TLP observation 33 Bode, J. E. 156, 224 nomenclature 157 Barstow, M. 303 Bode’s galaxy M81 362 notable (table) 162 Barwell meteorite 279, 282 Bode’s Law (table) 157 numbers of 156 my investigations 286 Bode’s Law 156, 245 orbits of 163 Barycentre, the 26 Boethin’s comet 269 potentially hazardous, list 169 Bauersfeld, W., Zeiss Planetarium 516 Bok globules 301, 352 satellites of 173 Bayer 349 Bok, Bart 301 searches, professional teams 162 Beagle 2 lander 141 Boles, Tom 335 space missions to 171 Beagle 2, failure of 141 Bolides 273 total mass of 156 Becker, A. and N. Kaib, discovery of 2006 272 254 Bond, G. P 20 Trojans (table) 176 Beckman, J. 20 Bond, W. and G. 203 Trojans 156 Beddgellert meteorite 282 Bondi, H. 365 vermin of the skies 156 Bedout High crater 286 Boomerang 364 Astraea 156 Australia 122 nebula 350 Astrometric binaries 319 Beer and Madler 127 Boo¨tes 387 Astronomers (list) 536–52 lunar map by 28 Borrelly’s Comet 268 Astronomers Royal (table) 508 Belt of Venus 291 Boulby Mine, Yorkshire, search for WIMPS 507 Astronomers Royal for Scotland (table) 508 Bennett’s comet 1970 270 Bovedy meteorite 282, 287 Astronomical nicknames (table) 339 mistaken as Israli war weapon 255 Boxhole crater, Australia 285 Astronomical Unit 1 Beppo Sax, gamma rays 518 Brandes and Benzenberg, meteor heights 273 Astronomy, history of 526 Berkovski, M. 23 Brezhina, A. 280 Atacama Desert observatories 507 Bessell, E. W., lunar measurements 28 Bright naked eye comets 1900–2010 271 Atalanta Regio 115 Bessell, F. W. 293 Britannica publication 1661 292 Atla Regio 115 and 61cygni 318 British Astronomical Association: Jupiter Atmosphere, lower, composition of Beta Pictoris, dust clouds around 522 Section 179 (table) 124 Beta Regio 115 British meteorites falls (table) 282 Atmosphere, structure of (table) 124 Betelgeux 304, 327 British Total Eclipses 23 Aumann, H. and P. Gillett 309 Bethe, H. 10, 301, 364 Brocchi’s cluster 370 Auriga 385 Bianchini, map of Venus 1727 109 Bronzites 280 z Aurigae 324 Biela’s comet, D/3 264 Brookhaven National Laboratory 12 Aurorae 8 panic 1832 255 Brorsen, Theodor 292 and sunspots 289 Biermann, L. 17 Brown dwarfs 302, 309 Australis 508 Big Bang 357 Buffham, J. 225 described by Fridtjof Nansen 290 term by Fred Hoyle 363 Buffon, conte de 121 in southern England 289 Big Crunch 365 Bug nebula 351 on other worlds 290 Bigg, K. E. and Jupiter’s radio waves 184 Buie, Marc, and surface of Pluto 248 Planum 137 Binary stars, spectroscopic binaries 318 Bunsen, R. 9 Aurorae, altitudes 289 Binary systems 293 Buren, Godfried 24 brilliance of (table) 290 numbers 318 Burgasser, A. 302 causes of 289 origins 319 Burke, B. and K. Franklin, radio waves colours of 290 postulated in 1766 318 from Jupiter 184 form and brilliance 289 types 319 Burney, Venetia, naming of Pluto 246 frequency 289 Biot, J. B., meteor shower at L’Aigle 280 Burnham, S. W. 315 legends and folklore 288 Birkeland, K. 289 Burnright, R. 519 odours from 290 Birr telescope 357 Bush, George W. 121 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-89935-2 - Patrick Moore’s Data Book of Astronomy Edited by Patrick Moore and Robin Rees Index More information 562 Index Butterfly diagram, the 9 Centaurus A 360, 362, 520 Climate, variations in 125 Buvard, A., tables of Uranus 235 Centaurus X3 520 Cloverleaf 361 Centaurus Clusters and nebulae, first known (table) 339 Caelum 389 Omega Centauri black hole 307 CME 17 Caldwell catalogue 343–6 a Centauri 293, 309, 315 Coal Sack C90 nebula 352 Calendars, early 526 Cepheid period luminosity law 356 Coal Sack C99 353 Calichus, Andreas and comets 255 variables 303 COBE (Cosmic Background Explorer Callisto variables 328 Satellite) 364 Catenae 199 Cepheus 406 Coblenz and Lampland ‘violet layer of ’ 131 constitution of 199 g Cephei, presence of planet? 309 Cockell, C., Forward to Mars party 131 map 198 m Cephei (Garnet Star) 327 Colette, Aphrodite Terra 115 outer satellites of 199 Cerdic, King 22 Collins, S. 209 outermost Galilean 197 Cerenkov radiation 12 Colombo gap 203 possible underground ocean 199 Ceres 156, 166 Columba 411 ringed basins, Valhalla and Asgard 199 Cerro Tololo 302 Coma Berenices 412 small outer satellites: Themisto, Pasiphae, observatory 327 Comas Sola, J.
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    Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED
  • The Comet's Tale, and Therefore the Object As a Whole Would the Section Director Nick James Highlighted Have a Low Surface Brightness

    The Comet's Tale, and Therefore the Object As a Whole Would the Section Director Nick James Highlighted Have a Low Surface Brightness

    1 Diebold Schilling, Disaster in connection with two comets sighted in 1456, Lucerne Chronicle, 1513 (Wikimedia Commons) THE COMET’S TALE Comet Section – British Astronomical Association Journal – Number 38 2019 June britastro.org/comet Evolution of the comet C/2016 R2 (PANSTARRS) along a total of ten days on January 2018. Composition of pictures taken with a zoom lens from Teide Observatory in Canary Islands. J.J Chambó Bris 2 Table of Contents Contents Author Page 1 Director’s Welcome Nick James 3 Section Director 2 Melvyn Taylor’s Alex Pratt 6 Observations of Comet C/1995 01 (Hale-Bopp) 3 The Enigma of Neil Norman 9 Comet Encke 4 Setting up the David Swan 14 C*Hyperstar for Imaging Comets 5 Comet Software Owen Brazell 19 6 Pro-Am José Joaquín Chambó Bris 25 Astrophotography of Comets 7 Elizabeth Roemer: A Denis Buczynski 28 Consummate Comet Section Secretary Observer 8 Historical Cometary Amar A Sharma 37 Observations in India: Part 2 – Mughal Empire 16th and 17th Century 9 Dr Reginald Denis Buczynski 42 Waterfield and His Section Secretary Medals 10 Contacts 45 Picture Gallery Please note that copyright 46 of all images belongs with the Observer 3 1 From the Director – Nick James I hope you enjoy reading this issue of the We have had a couple of relatively bright Comet’s Tale. Many thanks to Janice but diffuse comets through the winter and McClean for editing this issue and to Denis there are plenty of images of Buczynski for soliciting contributions. 46P/Wirtanen and C/2018 Y1 (Iwamoto) Thanks also to the section committee for in our archive.
  • ESO's VLT Sphere and DAMIT

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    ESO’s VLT Sphere and DAMIT ESO’s VLT SPHERE (using adaptive optics) and Joseph Durech (DAMIT) have a program to observe asteroids and collect light curve data to develop rotating 3D models with respect to time. Up till now, due to the limitations of modelling software, only convex profiles were produced. The aim is to reconstruct reliable nonconvex models of about 40 asteroids. Below is a list of targets that will be observed by SPHERE, for which detailed nonconvex shapes will be constructed. Special request by Joseph Durech: “If some of these asteroids have in next let's say two years some favourable occultations, it would be nice to combine the occultation chords with AO and light curves to improve the models.” 2 Pallas, 7 Iris, 8 Flora, 10 Hygiea, 11 Parthenope, 13 Egeria, 15 Eunomia, 16 Psyche, 18 Melpomene, 19 Fortuna, 20 Massalia, 22 Kalliope, 24 Themis, 29 Amphitrite, 31 Euphrosyne, 40 Harmonia, 41 Daphne, 51 Nemausa, 52 Europa, 59 Elpis, 65 Cybele, 87 Sylvia, 88 Thisbe, 89 Julia, 96 Aegle, 105 Artemis, 128 Nemesis, 145 Adeona, 187 Lamberta, 211 Isolda, 324 Bamberga, 354 Eleonora, 451 Patientia, 476 Hedwig, 511 Davida, 532 Herculina, 596 Scheila, 704 Interamnia Occultation Event: Asteroid 10 Hygiea – Sun 26th Feb 16h37m UT The magnitude 11 asteroid 10 Hygiea is expected to occult the magnitude 12.5 star 2UCAC 21608371 on Sunday 26th Feb 16h37m UT (= Mon 3:37am). Magnitude drop of 0.24 will require video. DAMIT asteroid model of 10 Hygiea - Astronomy Institute of the Charles University: Josef Ďurech, Vojtěch Sidorin Hygiea is the fourth-largest asteroid (largest is Ceres ~ 945kms) in the Solar System by volume and mass, and it is located in the asteroid belt about 400 million kms away.
  • Observation of Near-Earth Object (1566) Icarus and the Split Candidate 2007 MK6

    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.
  • CAPTURE of TRANS-NEPTUNIAN PLANETESIMALS in the MAIN ASTEROID BELT David Vokrouhlický1, William F

    CAPTURE of TRANS-NEPTUNIAN PLANETESIMALS in the MAIN ASTEROID BELT David Vokrouhlický1, William F

    The Astronomical Journal, 152:39 (20pp), 2016 August doi:10.3847/0004-6256/152/2/39 © 2016. The American Astronomical Society. All rights reserved. CAPTURE OF TRANS-NEPTUNIAN PLANETESIMALS IN THE MAIN ASTEROID BELT David Vokrouhlický1, William F. Bottke2, and David Nesvorný2 1 Institute of Astronomy, Charles University, V Holešovičkách 2, CZ–18000 Prague 8, Czech Republic; [email protected] 2 Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302; [email protected], [email protected] Received 2016 February 9; accepted 2016 April 21; published 2016 July 26 ABSTRACT The orbital evolution of the giant planets after nebular gas was eliminated from the Solar System but before the planets reached their final configuration was driven by interactions with a vast sea of leftover planetesimals. Several variants of planetary migration with this kind of system architecture have been proposed. Here, we focus on a highly successful case, which assumes that there were once five planets in the outer Solar System in a stable configuration: Jupiter, Saturn, Uranus, Neptune, and a Neptune-like body. Beyond these planets existed a primordial disk containing thousands of Pluto-sized bodies, ∼50 million D > 100 km bodies, and a multitude of smaller bodies. This system eventually went through a dynamical instability that scattered the planetesimals and allowed the planets to encounter one another. The extra Neptune-like body was ejected via a Jupiter encounter, but not before it helped to populate stable niches with disk planetesimals across the Solar System. Here, we investigate how interactions between the fifth giant planet, Jupiter, and disk planetesimals helped to capture disk planetesimals into both the asteroid belt and first-order mean-motion resonances with Jupiter.
  • Adaptive Optics Observations of Asteroid (216) Kleopatra

    Adaptive Optics Observations of Asteroid (216) Kleopatra

    A&A 394, 339–343 (2002) Astronomy DOI: 10.1051/0004-6361:20021094 & c ESO 2002 Astrophysics Research Note Adaptive optics observations of asteroid (216) Kleopatra D. Hestroffer1,F.Marchis2,, T. Fusco3, and J. Berthier1 1 IMCCE, UMR CNRS 8028, Paris Observatory, 77 Av. Denfert Rochereau, 75014 Paris, France 2 CFAO/University of California, Dept. of Astronomy, 601 Campbell Hall, Berkeley, CA 94720, USA 3 ONERA, DOTA-E, BP 72, 92322 Chˆatillon, France Received 22 March 2002 / Accepted 11 July 2002 Abstract. The large main-belt asteroid (216) Kleopatra has been for long suspected to be a binary object, mainly due to its large lightcurve amplitude. However, recent observations suggest that it is a single “bone-shaped” or bi-lobated body (Ostro et al. 2000; Tanga et al. 2001). We present results obtained from ground-based adaptive optics observations, and in agreement with the radar raw-observations, the images show two prominent lobes. Making use of the MISTRAL deconvolution technique, the restored images yield a well-separated binary object. Nevertheless, the spatial resolution of the 3.6 m ESO telescope is limited and a dumbbell-shaped body could yield similar features. Further simulations show that adaptive optics observations with an 8-meter class telescope analyzed with the powerful MISTRAL deconvolution technique could overcome this limitation. Key words. instrumentation: adaptive optics – minor planets, asteroids 1. Introduction provide additional constraints on collisional-evolution and binary-formation models. At the beginning of last century, by analyzing the asteroid Direct or indirect imaging of Kleopatra in the past showed (433) Eros, Andr´e made the hypothesis that asteroids could it to be a very elongated body but was not able to conclusively have satellites (Andr´e 1901).
  • Dynamical Evolution of the Cybele Asteroids

    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

    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.
  • (704) Interamnia from Its Occultations and Lightcurves

    (704) Interamnia from Its Occultations and Lightcurves

    International Journal of Astronomy and Astrophysics, 2014, 4, 91-118 Published Online March 2014 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2014.41010 A 3-D Shape Model of (704) Interamnia from Its Occultations and Lightcurves Isao Satō1*, Marc Buie2, Paul D. Maley3, Hiromi Hamanowa4, Akira Tsuchikawa5, David W. Dunham6 1Astronomical Society of Japan, Yamagata, Japan 2Southwest Research Institute, Boulder, USA 3International Occultation Timing Association, Houston, USA 4Hamanowa Astronomical Observatory, Fukushima, Japan 5Yanagida Astronomical Observatory, Ishikawa, Japan 6International Occultation Timing Association, Greenbelt, USA Email: *[email protected], [email protected], [email protected], [email protected], [email protected], [email protected] Received 9 November 2013; revised 9 December 2013; accepted 17 December 2013 Copyright © 2014 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract A 3-D shape model of the sixth largest of the main belt asteroids, (704) Interamnia, is presented. The model is reproduced from its two stellar occultation observations and six lightcurves between 1969 and 2011. The first stellar occultation was the occultation of TYC 234500183 on 1996 De- cember 17 observed from 13 sites in the USA. An elliptical cross section of (344.6 ± 9.6 km) × (306.2 ± 9.1 km), for position angle P = 73.4 ± 12.5˚ was fitted. The lightcurve around the occulta- tion shows that the peak-to-peak amplitude was 0.04 mag. and the occultation phase was just be- fore the minimum.
  • Asteroid 1566 Icarus's Size, Shape, Orbit, and Yarkovsky Drift from Radar

    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.
  • 7 X 11 Long.P65

    7 X 11 Long.P65

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  • Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1

    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: [email protected]; 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: [email protected] 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.