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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 – Chair: Elbert Macau 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 1 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 – Chair: Juliano Oliveira 11:20 Sessão de pôsteres Mecânica orbital e Controle I (MOC I) 12:00 Almoço (14:20 – 16:20): Sessão 2 – Astronomia I - Chair: Sylvio Ferraz Mello 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 – Chair: Juliano Oliveira 17:40 Sessão de pôsteres Astronomia I (AST I) 19:00 Jantar. Quarta-feira, 30 de novembro Manhã: Sessão 3 – Sistemas Dinâmicos – Chair: Juliano Oliveira 2 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 – Chair: Juliano Oliveira 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 – Chair: Marisa Roberto 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 3 17:40 Sessão de pôsteres Geral 19:00 Jantar. Quinta-feira, 01 de dezembro Manhã: Sessão 5 – Astronomia II – Chair: Tadashi Yokoyama 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 – Chair: Antonio Bertachini 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 (INPE): Critical Applications of Fault Detection Isolation and Recovery for Spacecrat 15:40 – 16:00 Francisco J. T. Salazar (UNESP): Aproveitamento da energia solar por meio de espelhos espaciais 4 16:00 – 16:20 Leandro Baroni (UFABC): Filtro de Kalman para a determinação de atitude de um CubeSat usando sensores de baixo custo 16:20 – 16h40 Intervalo 16:40 – 17h40 (60 min): Georgi Smirnov (Palestrante convidado, Univ. do Minho/Portugal): Mathematical problems of orbital maneuvers with single-input control 17:40 Sessão de pôsteres Mecânica Orbital e Controle II (MOC II) 19:00 Jantar. Sexta-feira, 02 de dezembro Manhã: Sessão 7 – Astronomia III – Chair: Maria Helena Morais 8:00 – 9:00 (60 min) Fathi Namouni (Palestrante convidado, Observ. “de la Côte d'Azur”/França): Resonance dynamics at arbitrary inclination 9:00 – 09:20 André Izidoro (CNRS): Making Planet-9 from the scattering of planetary cores during the accretion of Uranus and Neptune 9:20 – 09:40 Rodney da Silva Gomes (ON): A Inclinação do Eixo de Rotação do Sol pode ser explicada pela Presença de um Planeta Distante 9:40 – 10:00 Fernando V. Roig (ON): Formação de crateras de impacto nos planetas terrestres e na Lua durante a instabilidade dos planetas gigantes 10:00 – 10:20 Intervalo 10:20 – 10:40 Valério Carruba (UNESP): Detection of the YORP Effect for Small Asteroids in the Karin Cluster 11:00 Encerramento. 5 SESSÕES DE PÔSTERES Terça-feira, 29 de novembro Manhã: Sessão 1 – Mecânica orbital e Controle I 11:20 Sessão de pôsteres Mecânica orbital e Controle I (MOC I) Pôsteres MOC I-1 até 48 e MOC II-12 e SD-5 Tarde: Sessão 2 – Astronomia I 17:40 Sessão de pôsteres Astronomia I (AST I) Pôsteres AST I-1 até 31 e AST II-15 e AST II-16 Quarta-feira, 30 de novembro Manhã: Sessão 3 – Sistemas Dinâmicos 11:20 Sessão de pôsteres Sistemas Dinâmicos (SD) Pôsteres SD-1 até 12 Tarde 17:40 Sessão de pôsteres Geral Todas as áreas Quinta-feira, 01 de dezembro Manhã: Sessão 5 – Astronomia II 11:20 Sessão de pôsteres Astronomia II (AST II) Pôsteres AST II-1 até 36 Tarde: Sessão 6 – Mecânica Orbital e Controle III 17:40 Sessão de pôsteres Mecânica Orbital e Controle II (MOC II) Pôsteres MOC II-1 até 38 e MOC I-13 6 RESUMOS DOS TRABALHOS AST I-1 Evolução spin – órbita em sistemas de dois planetas usando modelo viscoelástico de deformação Adrián Rodríguez Colucci (1), Nelson Callegari Jr. (2), Alexandre Correia (3) (1) Observatório do Valongo – UFRJ, (2) DEMAC/UNESP, (3) Universidade de Aveiro Investigamos a evolução das órbitas e da rotação em sistemas de dois planetas que interagem mutuamente, assumindo que o planeta interno é deformado de forma viscoelástica pela força de maré da estrela central. A análise é feita através da resolução numérica das equações exatas do movimento e da deformação instantânea da figura do planeta. A aplicação ao sistema extrassolar CoRoT-7 mostra que, dependendo do tempo de relaxamento da deformação, a rotação do planeta interno pode ficar capturada em ressonância spin-órbita. Para tempos de relaxamento grandes, a excentricidade da órbita interna pode ser exitada e atingir grandes valores, podendo dar uma explicação às altas excentricidades observadas em alguns sistemas de super-Terras quentes com companheiros externos. Agradecimentos: Fapesp AST I-2 Uso de programação GPU para simulações em mecânica celeste Alan Costa de Souza (1), Fernando Roig (1) (1) Observatório Nacional Um dos objetivos da mecânica celeste é tentar prever o comportamento de um sistema de N corpos, no passado ou no futuro, evoluindo sob a ação de certas forças. Para tanto, é necessário conhecer a sua posição e velocidade no presente. Na maioria das vezes, a única alternativa para conseguir isto é utilizando simulações computacionais. Até meados dos anos 90 essas simulações eram realizadas de forma sequencial, porém, o surgimento de processadores multinúcleos tornou possível o desenvolvimento de algoritmos paralelos. Tais algoritmos são mais eficientes que os sequenciais, reduzindo o tempo total gasto nas simulações. 7 Diante disto, nesse trabalho vamos mostrar como uma implementação paralela em GPU[2] pode ser muito mais eficiente que uma implementação sequencial. A modo de exemplo, faremos uma comparação entre um código sequencial usando o algoritmo simplético de quarta ordem de Ruth[1] e a implementação do mesmo algoritmo usando GPU, executando numa placa gráfica inicialmente designada para execução de jogos de computador, mas que atualmente é usada para executar simulações massivamente paralelas em diversas áreas da ciência. Referências [1] Forest, Etienne e Ronald D. Ruth. "Fourth-order Symplectic integration. Physica D: Nonlinear Phenomena 43.1 (1990): 105-117. [2] https://developer.nvidia.com/cuda-zone Agradecimentos: CAPES, CNPq MOC I-1 Análise da sensibilidade dos parâmetros envolvidos em uma manobra de Swing-By propulsada Alessandra F.
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  • Perturbations in the Motion of the Quasicomplanar Minor Planets For

    Perturbations in the Motion of the Quasicomplanar Minor Planets For

    Publications of the Department of Astronom} - Beograd, N2 ID, 1980 UDC 523.24; 521.1/3 osp PERTURBATIONS IN THE MOTION OF THE QUASICOMPLANAR MI­ NOR PLANETS FOR THE CASE PROXIMITIES ARE UNDER 10000 KM J. Lazovic and M. Kuzmanoski Institute of Astronomy, Faculty of Sciences, Beograd Received January 30, 1980 Summary. Mutual gravitational action during proximities of 12 quasicomplanar minor pla­ nets pairs have been investigated, whose minimum distances were under 10000 km. In five of the pairs perturbations of several orbital elements have been stated, whose amounts are detectable by observations from the Earth. J. Lazovic, M. Kuzmanoski, POREMECAJI ELEMENATA KRETANJA KVAZIKOM­ PLANARNIH MALIH PLANETA U PROKSIMITETIMA NJIHOVIH PUTANJA SA DA­ LJINAMA MANJIM OD 10000 KM - Ispitali smo medusobna gravitaciona de;stva pri proksi­ mitetima 12 parova kvazikomplanarnih malih planeta sa minimalnim daljinama ispod 10000 km. Kod pet parova nadeni su poremecaji u vi~e putanjskih elemenata, ~iji bi se iznosi mogli ustano­ viti posmatranjima sa Zemlje. Earlier we have found out 13 quasicomplanar minor planets pairs (the angle I between their orbital planes less than O~500), whose minimum mutual distances (pmin) were less than 10000 km (Lazovic, Kuzmanoski, 1978). The shortest pro­ ximity distance of only 600 km among these pairs has been stated with minor planet pair (215) Oenone and 1851 == 1950 VA. The corresponding perturbation effects in this pair have been calculated (Lazovic, Kuzmanoski, 1979a). This motivated us to investigate the mutual perturbing actions in the 12 remaining minor planets pairs for the case they found themselves within the proximities of their correspon­ ding orbits.
  • Orbital Stability Assessments of Satellites Orbiting Small Solar System Bodies a Case Study of Eros

    Orbital Stability Assessments of Satellites Orbiting Small Solar System Bodies a Case Study of Eros

    Delft University of Technology, Faculty of Aerospace Engineering Thesis report Orbital stability assessments of satellites orbiting Small Solar System Bodies A case study of Eros Author: Supervisor: Sjoerd Ruevekamp Jeroen Melman, MSc 1012150 August 17, 2009 Preface i Contents 1 Introduction 2 2 Small Solar System Bodies 4 2.1 Asteroids . .5 2.1.1 The Tholen classification . .5 2.1.2 Asteroid families and belts . .7 2.2 Comets . 11 3 Celestial Mechanics 12 3.1 Principles of astrodynamics . 12 3.2 Many-body problem . 13 3.3 Three-body problem . 13 3.3.1 Circular restricted three-body problem . 14 3.3.2 The equations of Hill . 16 3.4 Two-body problem . 17 3.4.1 Conic sections . 18 3.4.2 Elliptical orbits . 19 4 Asteroid shapes and gravity fields 21 4.1 Polyhedron Modelling . 21 4.1.1 Implementation . 23 4.2 Spherical Harmonics . 24 4.2.1 Implementation . 26 4.2.2 Implementation of the associated Legendre polynomials . 27 4.3 Triaxial Ellipsoids . 28 4.3.1 Implementation of method . 29 4.3.2 Validation . 30 5 Perturbing forces near asteroids 34 5.1 Third-body perturbations . 34 5.1.1 Implementation of the third-body perturbations . 36 5.2 Solar Radiation Pressure . 36 5.2.1 The effect of solar radiation pressure . 38 5.2.2 Implementation of the Solar Radiation Pressure . 40 6 About the stability disturbing effects near asteroids 42 ii CONTENTS 7 Integrators 44 7.1 Runge-Kutta Methods . 44 7.1.1 Runge-Kutta fourth-order integrator . 45 7.1.2 Runge-Kutta-Fehlberg Method .
  • A Low Density of 0.8 G Cm-3 for the Trojan Binary Asteroid 617 Patroclus

    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.