DOCSLIB.ORG

Soc) Comitê Organizador Local (Loc

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Soc) Comitê Organizador Local (Loc COMITÊ CIENTÍFICO (SOC) Adrián Rodríguez Colucci – Observatório do Valongo/RJ/UFRJ Antonio F. Bertachini A. Prado – INPE/São José dos Campos Carlos Tabaré Gallardo – Departamento de Astronomia/Universidad de la Republica/Uruguai Elbert E. N. Macau – INPE Ernesto Vieira Neto – Faculdade de Engenharia (FEG)/ Unesp Campus Guaratingetá Iberê Luiz Caldas – Instituto de Física/Universidade de São Paulo (USP) Nelson Callegari Júnior – (Coordenador) Instituto de Geociências e Ciências Exatas (IGCE), Unesp/Campus Rio Claro Ricardo Egydio de Carvalho – IGCE Sylvio Ferraz-Mello – Instituto de Astronomia, Geofísica e Ciências Atmosféricas/USP Tadashi Yokoyama – IGCE COMITÊ ORGANIZADOR LOCAL (LOC) Edson Denis Leonel – IGCE José Leonardo Ferreira – Instituto de Física/ Universidade de Brasília Julio Camargo – Observatório Nacional/RJ Maria Helena M. Morais – IGCE Rafael Sfair – FEG Silvia Giuliatti Winter – FEG Site do Evento 2016 http://igce.rc.unesp.br/departamentos/demac/docentes/cbdo18/ 1 HISTÓRICO DO CBDO Os Colóquios Brasileiros de Dinâmica Orbital se realizam a cada dois anos, desde 1982. O primeiro CBDO, realizado no ITA em julho de 1982, foi organizado por iniciativa do Dr. Wagner Sessin, e tinha como finalidade principal reunir pesquisadores das áreas astronômica e espacial, interessados nos problemas de Mecânica Celeste Pura e Aplicada. Esse colóquio não recebeu a denominação genérica dos demais, iniciada a partir do segundo colóquio. O primeiro colóquio teve como título: “Movimentos de Satélites Artificiais: Teoria, Determinação e Aplicações” e dele participaram 51 pesquisadores e pós-graduandos de vários estados brasileiros: São Paulo, Rio de Janeiro, Paraná, Minas Gerais e Pernambuco. Para mais detalhes das realizações do Evento, ver http://www.astro.iag.usp.br/~dinamica/cbdo.htm A atual edição do CBDO conta com 200 atividades inscritas, divididas nos seguintes formatos: Apresentações orais de palestrantes convidados do exterior e do Brasil: 14 Apresentações orais de palestrantes selecionados pelo Comitê Científico: 22 Comunicações em formato pôster: 164 Índice Este livro de resumos contém: Homenagem ao Prof. Sylvio Ferraz-Mello……….. Pg 003 Quadro de Programação………………….……….. Pg 004 Programação detalhada das comunicações....….. Pg 005 Sessões de pôsteres........................................…. Pg 010 Lista dos Participantes......................................…. Pg 011 Resumos dos trabalhos....................................…. Pg 023 Índice dos Autores e Coautores..........................… Pg 222 Agências Financiadoras.....................................… Pg 233 2 HOMENAGEM AO PROF. SYLVIO FERRAZ-MELLO Sylvio Ferraz-Mello nasceu em São Paulo em 26/10/1936. Concluiu a Graduação em Física pela Universidade de São Paulo (USP) em 1959, e o Doutorado em Ciências Matemáticas pela Universidade de Paris em 1967. Foi professor pleno do Instituto Tecnológico da Aeronáutica e professor titular do Instituto de Astronomia, Geofísica e Ciências Atmosféricas da USP, do qual também foi diretor. Ocupou posições temporárias nas Universidades de Paris, La Plata, Porto, Viena, Texas e no Observatório de Nice. Foi diretor do Observatório Nacional, membro do Conselho da Academia de Ciências da América Latina, presidente da Comissão 7 da União Astronômica Internacional (IAU) e presidente da Sociedade Astronômica Brasileira (SAB), da qual também é sócio fundador. Atualmente é professor emérito da USP, editor-chefe da revista Celestial Mechanics and Dynamical Astronomy, e membro da Academia Brasileira de Ciências. Entre outros prêmios, foi agraciado com a Grã-Cruz da Ordem Nacional do Mérito Científico, o título de Doutor Honoris Causa do Observatório de Paris, e o Prêmio Brouwer da Divisão de Astronomia Dinâmica da Sociedade Astronômica Americana. O asteroide (5201) 1983 XF foi rebatizado com seu nome pela IAU. Até o presente, as suas pesquisas abrangeram diversos tópicos tais como dinâmica de satélites artificiais e satélites galileanos, teoria de perturbações, análise de séries temporais, ressonâncias e caos em sistemas planetários, dinâmica de asteroides, caracterização de exoplanetas e forças de maré. Ao longo da sua profícua carreira publicou mais de 130 artigos em periódicos especializados internacionais, diversos livros e capítulos de livros, entre os que se destaca o livro Canonical Pertubation Theories, Degenerate Systems and Resonances, e formou mais de 35 doutores e mestres. Foi um dos idealizadores, junto a Wagner Sessin e Atair Rios Neto, dos Colóquios Brasileiros de Dinâmica Orbital. Seu trabalho de pesquisa e de formação de jovens cientistas continua incansável até os dias de hoje. 3 QUADRO DE PROGRAMAÇÃO 4 PROGRAMAÇÃO DO CBDO 2016 Segunda-feira, 28 de novembro 08:00 – 12:00 Inscrições, entrega de material 14:20 Cerimônia de Abertura do XVIII CBDO 14:40 Cerimônia de Homenagem ao Prof. Sylvio Ferraz-Mello (Fernando V. Roig - ON) 15:30 Palestra de Abertura – Sylvio Ferraz-Mello (USP): Marés anelásticas em satélites e exoplanetas 16:30 Intervalo 16:45 Entrega do Prêmio Wagner Sessin 17:00 – 17h30 Palestrante Vencedor Categoria Astronomia Dinâmica e Planetária: F. Braga-Ribas (UTFPR): Ocultação estelar pelo satélite Vanth (Orcus/1): primeira predição e detecção 17:30 – 18h00 Palestrante Vencedor Categoria Mecânica Orbital e Controle: Diogo Merguizo Sanchez (INPE): On the use of perturbation maps in Astrodynamics and Celestial Mechanics 18:40 Coquetel de recepção. 19:40 Jantar. Terça-feira, 29 de novembro (8:20 – 10:00): Sessão 1 – Mecânica orbital e Controle I 8:20 – 9:20 (60 min) Kathleen Connor Howell (Palestrante convidado, Univ. de Purdue/EUA): Dynamical Systems Methods Applied to Spacecraft Trajectory Design 9:20 – 09:40 Priscilla A. de Sousa-Silva (ITA): Fast low-cost Earth-Moon transfers: a new strategy to compute optimal solutions using patched three- body systems 5 9:40 – 10:00 Jean Carvalho (UFRB): Effects of the solar radiation pressure and the nonsphericity of the planet (J2, J3, C22) in frozen orbits around mercury 10:00 – 10:20 Intervalo 10:20 – 11:20 (60 min) Celso Grebogi (Palestrante convidado, Univ. de Aberdeen/Escócia): Minicurso – Sistemas Dinâmicos, Parte 1: Transient Chaos 11:20 Sessão de pôsteres Mecânica orbital e Controle I (MOC I) 12:00 Almoço (14:20 – 16:20): Sessão 2 – Astronomia I 14:20 – 15:20 (60 min) Hauke Hussmann (Palestrante convidado, Centro Aeroespacial/Alemanha): Interior Structure and Dynamics of Satellites in the Outer Solar System 15:20 – 15:40 Hugo Folonier (USP): Titan's Length-of-Day Variation 15:40 – 16:00 Leonardo D.S. Trotta (UNESP): Modelo Dinâmico 3-d para a evolução do sistema Plutão-Caronte 16:00 – 16:20 Rafael Sfair (UNESP): O anel coorbital a Janus e Epimetheus 16:00 – 16h20 Intervalo 16:40 – 17h40 (60 min): Celso Grebogi (Palestrante convidado, Univ. de Aberdeen/Escócia): Minicurso – Sistemas Dinâmicos, Parte 2: Compressive sensing based prediction of complex dynamics and complex networks 17:40 Sessão de pôsteres Astronomia I (AST I) 19:00 Jantar. Quarta-feira, 30 de novembro Manhã: Sessão 3 – Sistemas Dinâmicos 8:00 – 9:00 (60 min) Celso Grebogi (Palestrante convidado, Univ. de Aberdeen/Escócia): Minicurso – Sistemas Dinâmicos, Parte 3: Tipping Point in Networked Dynamical Systems 6 9:00 – 09:20 Teresa J. Stuchi (UFRJ): Não Integrabilidade do hamiltoniano de Armburster-Gukenheimer-Kim com a teoria de Morales-Ramis 9:20 – 09:40 Marisa Roberto (ITA): Tokamaks com desviadores poloidais 9:40 – 10:00 R. Egydio de Carvalho (UNESP): Robust attractor of non-twist systems 10:00 – 10:20 Intervalo 10:20 – 11:20 (60 min) Ricardo Viana (Palestrante convidado, UFPR): Fractal structures in nonlinear plasma physics 11:20 Sessão de pôsteres Sistemas Dinâmicos (SD) 12:00 Almoço Tarde: Sessão 4 – Mecânica Orbital e Controle II 14:20 – 15:20 (60 min) Hauke Hussmann (Palestrante convidado, Centro Aeroespacial/Alemanha): Laser Altimetry in Planetary Applications 15:20 – 15:40 Jânia Duha (IFPR): The Yarkovsky-Duha effect and the unexpected strong correlation of thermal force with infrared radiation source colatitude 15:40 – 16:00 Jarbas Cordeiro Sampaio (IFBA): Space Debris in the neighborhood of operation artificial satellites 16:00 – 16:20 Liana Dias Gonçalves (INPE): Trajetórias na vizinhança de Fobos visando sobrevoo e aproximação 16:20 – 16h40 Intervalo 16:40 – 17h40 (60 min) Alexander A. Sukhanov (Palestrante convidado, Inst.de Ciências Espaciais/Rússia): Aster Project: First Brazilian Mission to Deep Space 17:40 Sessão de pôsteres Geral 19:00 Jantar. 7 Quinta-feira, 01 de dezembro Manhã: Sessão 5 – Astronomia II 8:00 – 9:00 (60 min) Tabaré Gallardo (Palestrante convidado, Univ. da República/Uruguai): Dynamics of high perihelion Transneptunian Objects 9:00 – 09:20 Carolina Charalambous (UNC/Argentina): Planetary migration and the origin of the 2/1 and 3/2 (near)-resonant population of close-in exoplanets 9:20 – 09:40 Eduardo S. G. Leandro (UFPE): Fatoração do Polinômio de Estabilidade de um Sistema Anular de N Corpos 9:40 – 10:00 Marcelo Assafin (ON): Predição do Ocultações Estelares por Satélites Irregulares até 2020 10:00 – 10:20 Intervalo 10:20 – 11:20 (60 min) Valéry Lainey (Palestrante convidado, Observatório de Paris/França): Quantification of tidal dissipation among giant planets from astrometry 11:20 Sessão de pôsteres Astronomia II (AST II) 12:00 Almoço Tarde: Sessão 6 – Mecânica Orbital e Controle III 14:20 – 15:20 (60 min) Mitchell L. R. Walker (Palestrante convidado, Inst. de Tecnologia da Geórgia/EUA): Unique Applications of Electric Propulsion 15:20 – 15:40 Ijar M. da Fonseca
Load more

Recommended publications
  • An Anisotropic Distribution of Spin Vectors in Asteroid Families
    Astronomy & Astrophysics manuscript no. families c ESO 2018 August 25, 2018 An anisotropic distribution of spin vectors in asteroid families J. Hanuš1∗, M. Brož1, J. Durechˇ 1, B. D. Warner2, J. Brinsfield3, R. Durkee4, D. Higgins5,R.A.Koff6, J. Oey7, F. Pilcher8, R. Stephens9, L. P. Strabla10, Q. Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, Ngunnawal ACT 2913, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), Italy Received x-x-2013 / Accepted x-x-2013 ABSTRACT Context. Current amount of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study not only the spin-vector properties of the whole population of MBAs, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the HCM method as members of ten collisional families, among them are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes.
    [Show full text]
  • 1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
    Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H.
    [Show full text]
  • The Three-Dimensional Structure of the Zodiacal Dust Bands
    ICARUS 127, 461±484 (1997) ARTICLE NO. IS975704 The Three-Dimensional Structure of the Zodiacal Dust Bands William T. Reach Universities Space Research Association and NASA Goddard Space Flight Center, Code 685, Greenbelt, Maryland 20771, and Institut d'Astrophysique Spatiale, BaÃtiment 121, Universite Paris XI, 91405 Orsay Cedex, France E-mail: [email protected] Bryan A. Franz General Sciences Corporation, NASA Goddard Space Flight Center, Code 970.1, Greenbelt, Maryland 20771 and Janet L. Weiland Hughes STX, NASA Goddard Space Flight Center, Code 685.9, Greenbelt, Maryland 20771 Received July 18, 1996; revised January 2, 1997 model, the dust is distributed among the asteroid family mem- Using observations of the infrared sky brightness by the bers with the same distributions of proper orbital inclination Cosmic Background Explorer (COBE)1 Diffuse Infrared Back- and semimajor axis but a random ascending node. In the mi- ground Experiment (DIRBE) and Infrared Astronomical Satel- grating model, particles are presumed to be under the in¯uence lite (IRAS), we have created maps of the surface brightness of Poynting±Robertson drag, so that they are distributed Fourier-®ltered to suppress the smallest (, 18) structures and throughout the inner Solar System. The migrating model is the large-scale background (.158). Dust bands associated with better able to match the parallactic variation of dust-band lati- the Themis, Koronis, and Eos families are readily evident. A tude as well as the 12- to 60-mm spectrum of the dust bands. dust band associated with the Maria family is also present. The The annual brightness variations can be explained only by the parallactic distances to the emitting regions of the Koronis, migrating model.
    [Show full text]
  • Asteroid Family Physical Properties, Numerical Sim- Constraints on the Ages of Families
    Asteroid Family Physical Properties Joseph R. Masiero NASA Jet Propulsion Laboratory/Caltech Francesca DeMeo Harvard/Smithsonian Center for Astrophysics Toshihiro Kasuga Planetary Exploration Research Center, Chiba Institute of Technology Alex H. Parker Southwest Research Institute An asteroid family is typically formed when a larger parent body undergoes a catastrophic collisional disruption, and as such family members are expected to show physical properties that closely trace the composition and mineralogical evolution of the parent. Recently a number of new datasets have been released that probe the physical properties of a large number of asteroids, many of which are members of identified families. We review these data sets and the composite properties of asteroid families derived from this plethora of new data. We also discuss the limitations of the current data, and the open questions in the field. 1. INTRODUCTION techniques that rely on simulating the non-gravitational forces that depend on an asteroid’s albedo, diameter, and Asteroid families provide waypoints along the path of density. dynamical evolution of the solar system, as well as labo- In Asteroids III, Zappala` et al. (2002) and Cellino et ratories for studying the massive impacts that were com- al. (2002) reviewed the physical and spectral properties mon during terrestrial planet formation. Catastrophic dis- (respectively) of asteroid families known at that time. Zap- ruptions shattered these asteroids, leaving swarms of bod- pala` et al. (2002) primarily dealt with asteroid size distri- ies behind that evolved dynamically under gravitational per- butions inferred from a combination of observed absolute turbations and the Yarkovsky effect to their present-day lo- H magnitudes and albedo assumptions based on the subset cations, both in the Main Belt and beyond.
    [Show full text]
  • Physical and Dynamical Properties of Asteroid Families
    Zappalà et al.: Properties of Asteroid Families 619 Physical and Dynamical Properties of Asteroid Families V. Zappalà, A. Cellino, A. Dell’Oro Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Torino P. Paolicchi University of Pisa The availability of a number of statistically reliable asteroid families and the independent confirmation of their likely collisional origin from dedicated spectroscopic campaigns has been a major breakthrough, making it possible to develop detailed studies of the physical properties of these groupings. Having been produced in energetic collisional events, families are an invaluable source of information on the physics governing these phenomena. In particular, they provide information about the size distribution of the fragments, and on the overall properties of the original ejection velocity fields. Important results have been obtained during the last 10 years on these subjects, with important implications for the general understanding of the collisional history of the asteroid main belt, and the origin of near-Earth asteroids. Some important problems have been raised from these studies and are currently debated. In particular, it has been difficult so far to reconcile the inferred properties of family-forming events with current understanding of the physics of catastrophic collisional breakup. Moreover, the contribution of families to the overall asteroid inventory, mainly at small sizes, is currently controversial. Recent investigations are also aimed at understanding which kind of dynamical evolution might have affected family members since the time of their formation. In addition to potential consequences on the interpretation of current data, there is some speculative possibility of obtaining some estimate of the ages of these groupings.
    [Show full text]
  • V-Type Candidates and Vesta Family Asteroids in the Moving Objects VISTA (MOVIS) Catalogue J
    Astronomy & Astrophysics manuscript no. 29465_hk_article c ESO 2021 July 27, 2021 V-type candidates and Vesta family asteroids in the Moving Objects VISTA (MOVIS) Catalogue J. Licandro1; 2, M. Popescu3; 4, D. Morate1; 2, and J. de León1; 2 1 Instituto de Astrofísica de Canarias (IAC), CVía Láctea sn, 38205 La Laguna, Spain 2 Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain 3 Astronomical Institute of the Romanian Academy, 5 Cu¸titulde Argint, 040557 Bucharest, Romania 4 Institut de Mécanique Céleste et de Calcul des Éphémérides (IMCCE) CNRS-UMR8028, Observatoire de Paris, 77 avenue Denfert- Rochereau, 75014 Paris Cedex, France Start working 01 May 2015 ABSTRACT Context. Basaltic asteroids (spectrally classified as V-types) are believed to be fragments of large differentiated bodies. The majority of them are found in the inner part of the asteroid belt, and are current or past members of the Vesta family. Recently, some V-type asteroids have been discovered far from the Vesta family supporting the hypothesis of the presence of multiple basaltic asteroids in the early solar system. The discovery of basaltic asteroids in the outer belt challenged the models of the radial extent and the variability of the temperature distribution in the early solar system. Aims. We aim to identify new basaltic V-type asteroids using near-infrared colors of ∼ 40000 asteroids observed by the VHS-VISTA survey and compiled in the MOVIS-C catalogue. We also want to study their near-infrared colors and to study the near-infrared color distribution of the Vesta dynamical family. Methods.
    [Show full text]
  • SDSS-Based Taxonomic Classification and Orbital Distribution of Main Belt Asteroids
    A&A 510, A43 (2010) Astronomy DOI: 10.1051/0004-6361/200913322 & c ESO 2010 Astrophysics SDSS-based taxonomic classification and orbital distribution of main belt asteroids J. M. Carvano1, P. H. Hasselmann1,2, D. Lazzaro1, and T. Mothé-Diniz2 1 Observatório Nacional (COAA), rua Gal. José Cristino 77, São Cristóvão, CEP 20921-400 Rio de Janeiro RJ, Brazil e-mail: [email protected] 2 Universidade Federal do Rio de Janeiro/Observatório do Valongo, Lad.Pedro Antônio, 43, 20080-090 Rio de Janeiro, Brazil Received 18 September 2009 / Accepted 4 November 2009 ABSTRACT Aims. The present paper aims to derive a new classification scheme for SDSS MOC asteroid colors that is compatible with previous taxonomies based on spectroscopic data. The distribution of these can give important clues to the formation and evolution of this region of the Solar System, as well as to locate candidates with mineralogically interesting spectra for detailed observations. Methods. The methodology is based on the large database SDSS MOC4. Templates of the main taxonomic classes are derived and then used to classify the asteroid observations in the SDSS MOC4. The derived taxonomic scheme is compatible with the Bus taxonomy and is suitable to the peculiarities of the SDSS observations, in particular, the low spectral resolution. Results. Density maps of the seven classes defined by the method reproduce classical results for the background which is mainly dominated by the S p class in the inner belt and by the Xp and the Cp classes beyond 2.8 AU. It also shows new structures, such as the fact that the Xp and Cp seem evenly distributed in the inner belt while in the outer belt the S p class increase in density only at the location of asteroid families.
    [Show full text]
  • Mineralogical Characterization of Baptistina Asteroid Family: Implications for K/T Impactor Source
    Mineralogical Characterization of Baptistina Asteroid Family: Implications for K/T Impactor Source Vishnu Reddy1,2 Department of Space Studies, Room 520, Box 9008, University of North Dakota, Grand Forks, ND 58202, USA. Email: [email protected] Jorge M. Carvano Observatório Nacional (COAA), rua Gal. José Cristino 77, São Cristóvão, CEP20921-400 Rio de Janeiro RJ, Brazil. Daniela Lazzaro Observatório Nacional (COAA), rua Gal. José Cristino 77, São Cristóvão, CEP20921-400 Rio de Janeiro RJ, Brazil. Tatiana A. Michtchenko Institute for Astronomy, Geophysics, and Atmospheric Sciences, University of São Paulo, Brazil. Michael J. Gaffey1 Department of Space Studies, Room 518, Box 9008, University of North Dakota, Grand Forks, ND58202, USA. Michael S. Kelley1,3 Department of Geology and Geography, Box 8149, Georgia Southern University, Statesboro, GA 30460, USA. Thais Mothé Diniz1 Observatório do Valongo, Federal University of Rio de Janeiro, Rio de Janeiro, RJ, Brazil. Alvaro Alvarez Candal , Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago 19, Chile. Nicholas A. Moskovitz1 Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241, Broad Branch Road, Washington, DC 20008, USA Edward A. Cloutis Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, Manitoba, Canada R3B 2E9 Erin L. Ryan Department of Astronomy, University of Minnesota, MN 55455, USA 1 1 Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538
    [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]
  • Spectroscopic Properties of Asteroid Families
    Cellino et al.: Spectroscopic Properties of Asteroids 633 Spectroscopic Properties of Asteroid Families A. Cellino Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Torino S. J. Bus University of Hawai‘i A. Doressoundiram Observatoire de Paris–Meudon D. Lazzaro Observatório Nacional, Rio de Janeiro Asteroid families have been the target of several dedicated campaigns of spectroscopic obser- vations during the last 10 years. Preliminary studies were mainly devoted to obtain a confirma- tion of the cosmochemical reliability of groupings identified by purely statistical analyses of the distributions of objects in the space of the orbital proper elements. These early attempts led to some spectacular confirmations of the common collisional origin of some families, like that associated with 4 Vesta. Subsequently, spectroscopic investigations started to be mostly focused on the issue of characterizing the overall mineralogical compositions of different families, at the same time looking for possible evidence of thermal differentiation of the original parent bodies and for possible evidence of ongoing space-weathering processes. Spectroscopy has also proven to be crucially needed to identify likely interlopers that can seriously affect the derived size distributions of families and the reconstruction of the original fields of ejection velocity of the fragments. At the same time, spectroscopic properties have been recognized as an invaluable tool to assess the real memberships of families mutually overlapping in the space of proper elements. Moreover, spectroscopic surveys have in general been found to be an excellent comple- ment to conventional family searches purely based on the identification of concentrations of objects in the proper-element space. A challenging unsolved problem comes from the fact that several families have been found to exhibit peculiar spectroscopic properties.
    [Show full text]
  • Interpreting the Cratering Histories of Bennu, Ryugu, and Other Spacecraft-Explored Asteroids W
    Interpreting the Cratering Histories of Bennu, Ryugu, and Other Spacecraft-explored Asteroids W. Bottke, D. Vokrouhlický, R.-L. Ballouz, Olivier Barnouin, H. Connolly, C. Elder, S. Marchi, T. Mccoy, Patrick Michel, M. Nolan, et al. To cite this version: W. Bottke, D. Vokrouhlický, R.-L. Ballouz, Olivier Barnouin, H. Connolly, et al.. Interpreting the Cratering Histories of Bennu, Ryugu, and Other Spacecraft-explored Asteroids. Astronomical Journal, American Astronomical Society, 2020, 160 (1), pp.14. 10.3847/1538-3881/ab88d3. hal-02986182 HAL Id: hal-02986182 https://hal.archives-ouvertes.fr/hal-02986182 Submitted on 22 Dec 2020 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. 1 Interpreting the Cratering Histories of Bennu, Ryugu, 2 and Other Spacecraft-Explored Asteroids 3 4 W.F. Bottke1, D. Vokrouhlický2, R.-L. Ballouz3, O. S. Barnouin4, H. C. Connolly Jr.3, 5, C. 5 Elder6, S. Marchi1, T. J. McCoy7, P. Michel8, M. C. Nolan3, B. Rizk3, D. J. Scheeres9, S. R. 6 Schwartz3, K. J. Walsh1, D. S. Lauretta3 7 8 1Southwest Research Institute, Boulder, CO, USA ([email protected]) 9 2Institute of Astronomy, Charles University, V Holešovičkách 2, CZ-18000, Prague 8, Czech Republic 10 3Lunar & Planetary Laboratory, University of Arizona, Tucson, AZ, USA 11 4Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA 12 5Dept.
    [Show full text]
  • An Anisotropic Distribution of Spin Vectors in Asteroid Families⋆
    A&A 559, A134 (2013) Astronomy DOI: 10.1051/0004-6361/201321993 & c ESO 2013 Astrophysics An anisotropic distribution of spin vectors in asteroid families J. Hanuš1,M.Brož1,J.Durechˇ 1,B.D.Warner2, J. Brinsfield3,R.Durkee4, D. Higgins5,R.A.Koff6,J.Oey7, F. Pilcher8, R. Stephens9,L.P.Strabla10,Q.Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, ACT 2913 Ngunnawal, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), 25020 Brescia, Italy Received 30 May 2013 / Accepted 16 September 2013 ABSTRACT Context. The current number of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study the spin-vector properties of not only the whole population of main-belt asteroids, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the hierarchical clustering method (HCM) as members of ten col- lisional families, among which are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes.
    [Show full text]