Context: Slivan (2002) determined spin state of ten asteroids in the Koronis family. Surprisingly, all four asteroids with prograde sense of rotation were shown to have spin axes nearly parallel in the inertial space. All asteroids with retrograde sense of rotation had large obliquities and rotation periods either short or long. It was shown that Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect can explain all these peculiar facts. In particular, it drives spin axes of the prograde rotators to be captured in a secular spin-orbital resonance known as Cassini state 2. Vokrouhlický et al. (2002) dubbed these configurations "Slivan states". Aims: A question arises whether Slivan states could exist also in other regions of the main asteroid belt, in particular its inner part, where observations are most easily obtained. Here, however, dynamical difficulties arise due to convergence of the proper frequency s and the planetary frequency s6. We investigate possibilities of a long-term stable capture in the Slivan state in the inner part of the main belt. Method: We used SWIFT integrator to determine orbital evolution of selected asteroids in the inner part of the main belt. In the case of 20 Massalia, we observed the asteroid in 2011, and used these new data to help better solve the rotation state using the...

In this thesis, we study how the planetary migration affects asteroid families. We identify the families among the Trojans of Jupiter by analysing their properties in the space of resonant elements, the size-frequency distribution and the colour indices. The previously reported number of families (10) seems to be overestimated, our analysis indicates that there is only one collisional family among Trojans with the parent-body size DPB > 100 km. We also performed a simulation of the long-term orbital evolution of the Trojan families. We used a modified version of the SWIFT symplectic integrator where the migration is set analytically. We found that the families are unstable even in the late stages of the migration, when Jupiter and Saturn recede from their mutual 1:2 resonance. Hence, the families observed today must have been created after the planetary migration ended. In the last part of the work, we study a formation of asteroid families in the Main Belt during the Late Heavy Bombardement. We simulate perturbations induced by migrating planets in the "jumping Jupiter" scenario (Morbidelli et al., 2010) and we conclude that big families (DPB > 200 km) created during the bombardement should be observable today.

Desde a revisão taxonômica dos Ophidiasteridae por H. L. Clark (1921), em que 20 gêneros foram reconhecidos como válidos, vários novos gêneros e espécies foram incluídos nesta família, e os limites entre alguns deles se tornaram largamente arbitrários. Isso também se aplica a Narcissia Gray, 1840, cuja morfologia e taxonomia são, ainda hoje, muito malcompreendidas. Os principais objetivos desta pesquisa foram: revisar a taxonomia do gênero Narcissia ao longo de toda a sua área de distribuição, a partir de estudos morfológicos; redescrever e caracterizar, morfologicamente, Narcissia trigonaria Sladen, 1889 strictu senso; caracterizar, morfologicamente, N. canariensis (d\'Orbigny, 1839) e N. ahearnae Pawson, 2007, as duas espécies válidas mais semelhantes a N. trigonaria; rever a validade de N. trigonaria helenaeMortensen, 1933; rever a validade de N. gracilis malpeloensis Downey, 1975. Cercade 370 espécimes do gênero Narcissia foram analisados: dois indivíduos de N. ahearnae, 82 espécimes de N. canariensis, 44 de N. gracilis e 242 de N. trigonaria. O material que serviu de base para nossos estudos pertence às coleções de museus nacionais e estrangeiras. Aterminologia para estruturas morfológicas seguiu Clark (1921), Turner & Dearborn (1972),Clark e Downey (1992) e Gale (2011). As pedicelárias foram classificadas de acordo com Jangoux e Lambert (1988). Todas as estruturas morfológicas de importância taxonômica foram ilustradas. E, pela primeira vez, os caracteres internos deste grupo foram estudados, a partir de microscopia eletrônica e tomografia. Uma nova diagnose para o gênero Narcissia foi disponibilizada. Todas as espécies do gênero foram revisadas e morfologicamente redescritas. Narcissia trigonaria, descrita a partir de um juvenil, foi redescrita a partir de um exemplar adulto, proveniente da localidade tipo (Bahia). Narcissia ahearnae é considerada uma espécie válida, e N. canariensis e N. trigonaria entidades distintas. Narcissia trigonaria helenae foi colocada na sinonímia de N. trigonaria, e N. gracilis malpeloensis entrou para a sinonímia de N. gracilis. A classificação de Narcissia, dentro da Família Ophidiasteridae, foi contestada, a partir de caracteres morfológicos. Os dados obtidos neste trabalho são, de longe, os mais completos já adquiridos para o gênero Narcissia e, futuramente, podem servir de base para os estudos morfológicos de outros grupos da Classe Asteroidea. / Since the taxonomic revision of the Ophidiasteridae by H. L. Clark (1921), in which 20 genera were recognized as valid, several new genera and species were included in this family, and the boundaries between some of them became largely arbitrary. This also applies to Narcissia Gray,1840, whose morphology and taxonomy are still very poorly understood today. The main goals of this research were: review the taxonomy of the genus Narcissia, throughout its range of distribution, from morphological studies; redescribe and characterize, morphologically, N. trigonaria Sladen, 1889 str. s; characterize, morphologically, N. canariensis (d\'Orbigny, 1839) and N. ahearnae Pawson, 2007, the two valid species most similar to N. trigonaria; review the validity of N. trigonaria var. helenaeMortensen, 1933; review the validity of the N. gracilismalpeloensis Downey, 1975. About 370 specimens of the genus Narcissia were analyzed: two individuals of N. ahearnae, 82 specimens of N. canariensis, 44 of N. gracilis, and 242 of N. trigonaria. The material that has served as a basis for our studies belongs to the national and foreign collections. The terminology for morphological structures has followed Clark (1921), Turner & Dearborn (1972), Clark & Downey (1992) and Gale (2011). Pedicellariae were classified according to Jangoux & Lambert (1988). All morphological structures of taxonomic importance have been illustrated. And, for the first time, the internal characters of this group were studied, from electron microscopy and tomography. A new diagnosis for the genus Narcissia was constructed. All species of the genus were reviewed and morphologically redescribed. Narcissia trigonaria, described from a juvenile, was redescribed from an adult specimen, from the type locality (Bahia). Narcissia ahearnae is considered a valid species, and N. canariensis and N. trigonaria distinct entities. Narcissia trigonaria helenaewas placed in the synonymy of N. trigonaria, and N. gracilis malpeloensis into the synonymy of N. gracilis.The classification of Narcissia, within the Family Ophidiasteridae, was contested, frommorphological characters. The data set obtained in this work are, by far, the most complete already acquired within the genus Narcissia and, in the future, may serve as the basis for the morphological studies of other groups of the Asteroidea Class.

Resumo: A existência de satélites irregulares é um tema de interesse científico há muito tempo devido às suas características peculiares, isto é, órbitas bem excêntricas, distantes do planeta e geralmente com altas inclinações em relação ao plano equatorial de seu planeta, chegando a ser em grande parte retrógradas. A existência de famílias de satélites irregulares, caracterizadas pela semelhança dos elementos orbitais dos satélites que as compõem é, ainda hoje, um fato não explicado. Tais características sugerem que os satélites irregulares não tenham sido formados juntamente com os planetas que estes orbitam, como se acredita ser o caso dos satélites regulares. Deste modo, uma explicação coerente para a existência dos mesmos é a captura gravitacional de corpos, formados em outras regiões, a partir de órbitas heliocêntricas após a ocorrência de um encontro próximo com o planeta. Entretanto, sob a dinâmica do Problema Circular Restrito de Três Corpos - PCR3C - capturas gravitacionais têm carater temporário, o que torna necessária a existência de um mecanismo de captura auxiliar. Isto tem incentivado, por anos, à proposição de vários modelos para explicar a existência dos satélites irregulares através da captura gravitacional, dentre os quais três se destacam na literatura: Dissipação por arrasto em gás, Pull-down capture - captura por puxão, interação colisional ou por encontros próximos com satélites pré-existentes, capturas de planetesimais durante encontros planetários e captura de asteróides binários. Considerando a dinâmica de 4-Corpos, investigamos numericamente a viabilidade de um modelo no qual um ente de um asteróide binário é capturado após sofrer um encontro próximo com um Júpiter, avaliando as condições que propiciam a captura de cada um dos membros, realizando um mapeamento dos parâmetros de modo... (Resumo completo, clicar acesso eletrônico abaixo) / Abstract: The existence of irregular satellites has been the focus of scientific interest for many years. That is due to their peculiar orbital features, i.e., highly eccentric orbits, large distance from the planet and, usually, with high inclination and many of them are retrograde. There are very well characterized families of irregular satellites, whose origin were not explained yet. These features suggest that irregular satellites were not formed together with the planet, during its formation stage, as were the regular ones. Therefore, an explanation for their existence is the gravitational capture of asteroids, originally in heliocentric orbits, that had a close encounter with the planet. However, considering only the Restrict Three Body Problem dynamics, it is not possible to accomplish permanent captures, being necessary the existence of an auxiliary mechanism. Then, several models were proposed in order to generate a permanent capture. Among the most important we found Gas drag dissipation, Pull-down capture, collisional and close encounters interactions with regular satellites, capture during planetary encounters and capture of binary asteroids. The current research had assessed how viable is a 4-body mechanism in which a member body of a binary asteroid remain captured after a close encounter with Jupiter. In order to accomplish that, we have mapped a set o parameters in order to find the proper conditions to yield the capture of one member. From the main results it is shown a very well permanent capture probability of the minor member when the primordial binary asteroid disrupts at a suitable "quadrature" configuration. Finally, it is also shown that this capture mechanism is well explained through energy exchanges. / Orientador: Othon Cabo Winter / Coorientador: Ernesto Vieira Neto / Banca: Tadashi Yokoyama / Banca: Fernando Virgilio Roig / Mestre

Orientador: Ernesto Vieira Neto / Co orientador: Antônio Delson C. de Jesus / Banca: Rodney da Silva Gomes / Banca: Tadashi Yokoyama / Resumo: Neste trabalho, apresentamos um estudo sobre a formação dos satélites irregulares de Júpiter por meio da captura gravitacional de asteróides binários. Analisamos as condições de ruptura/captura para um dos membros de um asteróide binário após um encontro próximo com o planeta considerando um conjunto de condições iniciais do Modelo de Nice. O sistema integrado é composto por quatro corpos: Sol, Júpiter e os membros do asteróide binário. Analisamos também o efeito do achatamento do membro mais massivo do asteróide binário. Nos resultados apresentados é possível perceber a relevância das perturbações, devidas ao Sol e ao achatamento, nos processos de troca de energia e momento angular para que um membro do asteróide torne-se permanentemente capturado. As configurações finais dos asteróides capturados são compatíveis com os objetos reais observados. / Abstract: In this work, we present a study on the irregular Jupiter's satellites formation by gravitational capture of binay asteroids. We analyze the conditions of capture to one or two members of the binary asteroid after a close-approach wiht the planet considering a set of initial conditions derived from Nice Model. Our system is composed of four bodies: Sun, Jupiter and the members of the binary asteroid. We also analyzed the oblateness effect of the bigger member of binary asteroid. The presented results showed the relevance of perturbations, due to Sun and the oblateness, in the process of exchange of energy and angular momentum for a member of the asteroid who will become permanently captured. The final configuration of captured asteroids are compatible with the real objects observed. / Mestre

Orientador: Othon Cabo Winter / Banca: Rafael Sfair de Oliveira / Banca: Felipe Bragda Ribas / Resumo: Ocultações estelares de Chariklo em 2013 revelaram algo que era desconhecido até o momento: anéis de partículas em torno de um corpo celeste do Sistema Solar diferente de um planeta. Este fato despertou o interesse da comunidade científica a respeito de assuntos como, por exemplo, o processo de formação desses anéis, por quanto tempo eles existirão, qual a probabilidade de corpos como o de Chariklo possuírem anéis ou ainda como eles se mantêm estáveis ao redor de um pequeno objeto, se comparado aos planetas. Neste trabalho estamos interessados em determinar o modelo físico de Chariklo através da manutenção da estrutura atual dos anéis. Acreditamos que este centauro é um corpo semelhante a um elipsoide, entretanto não sabemos com exatidão as dimensões de seus semieixos físicos a, b e c. As razões entre os valores destes semieixos resultam em diferentes valores para os termos de achatamento e elipticidade de Chariklo, que podem ser representados pelos termos J 2 e C 22 em seu potencial gravitacional. Além de determinar os limites para a forma de Chariklo, queremos também estudar quais são os efeitos que o achatamento e elipticidade do corpo central provocam na dinâmica das partículas dos anéis. Para isso, fizemos simulações numéricas usando um integrador que leva em conta os termos relacionados aos coeficientes J 2 e C 22 . O sistema que integramos é composto por Chariklo sendo orbitado por uma partícula com aproximadamente a mesma distância em que estão os anéis, fazendo uso d... (Resumo completo, clicar acesso eletrônico abaixo) / Abstract: Chariklo's stellar occultations in 2013 revealed something that was unknown to date: particle rings around a celestial body of the Solar system other than a planet. This fact has aroused the interest of the scientific community on issues such as the process of forming these rings, how long they will exist, how likely Chariklo bodies are to have rings or how stable they are around of a small object, compared to the planets. In this work we are interested in determining Chariklo's physical model by maintaining the current structure of the rings. We believe that this centaur is a body similar to an ellipsoid, but we do not know exactly the dimensions of its physical axes a, b, and c. The ratios between the values of these semi axes result in different values for the Chariklo flattening and ellipticity terms which can be represented by the terms J2 and C22 in its gravitational potential. In addition to determining the limits for the Chariklo form, we also want to study the effects of flattening and ellipticity on the dynamics of ring particles. For this, we did numerical simulations using an integrator that takes into account the terms related to the coefficients J2 and C22. The system we integrate is composed of Chariklo being orbited by a particle approximately the same distance as the rings, making use of the orbital osculating elements. The objective of these simulations was to reproduce the physical characteristics of the rings obtained through stellar occultations, however ... (Complete abstract click electronic access below) / Mestre

The term “homeland security”, seems to have become synonymous with terrorism in the minds of the general public. However, there are other threats to the security of the United States homeland that can be just as, if not more, devastating than terrorism. Included among these other threats is the potential of an asteroid collision with Earth. Historically, asteroid impact events have been responsible for the devastation of our planet and many of the mass extinction events encountered throughout the geologic record. Knowledge of physical parameters such as structure and rotational dynamics of the asteroid are critical parameters in developing interception and deflection techniques, as well as assessing the risk associated with these bodies and mitigation planning in the event of impact. This thesis encompasses the study of eight potentially hazardous asteroids identified in conjunction with NASA’s OSIRIS REX Mission and observed via the Target Asteroid Project, along with observations from the Robotically Controlled Telescope, and the Asteroid Light Curve Database of Photometry. Photometric data was extracted from all observations. Rotation periods of each target were confirmed using Lomb-Scargle time series analysis, with possible secondary periods indicated in the cases of Hathor (2.2169 hours), Bede (161.1501 hours), and Phaethon (4.5563 hours). Shape models for 2002 FG7, 2004 JN13, and Icarus were produced using light curve inversion techniques These are believed to be the first such models for these asteroids.

A number of missions to comets and asteroids have been undertaken by major space organizations driving a need to accurately characterize their gravitational fields. This is complicated however by their irregular shapes. To accurately and safely navigate spacecraft in these environments, a simple point-mass gravity model is insufficient and instead higher-fidelity models are required. Several such models exist for this purpose but all posess drawbacks. Moreover, there are some applications for which the currently available models are not particular well suited. In this dissertation, numerical quadrature and curvilinear meshing techniques are applied to the small body gravity problem. The goal of this work is to to create a gravitational model suitable for integating large numbers of low altitude trajectories and rapidly characterizing the near-surface potential field. In total three new models are developed. The first applies two-dimensional quadrature formulas to calculate the gravitational field of an arbitrary triangular surface mesh. The second extends this result to curvilinear surface meshes that more accurately approximate the surface topology. The third applies three-dimensional quadrature to curvilinear tetrahedral meshes to generate accurate distributions of point-masses. The accuracy of the new models is fully characterized and simple relations are presented for predicting the error of integrated trajectories. The efficiency of the models is then compared to other high-fidelity models currently in use. The new models perform well between the body's circumsphere and a thin layer that surrounds the surface.

<p>The dynamical evolution of the spin axis direction due to gravitational and thermal factors is examined. It is found that the spin axis variations generally are regular and relatively small for the bodies in the asteroid main belt. There are also reasons to believe that this is the case for minor objects beyond the main belt. However, it is found that these regular variations are larger when the orbital inclination of the objects is increased. This effect may explain certain features in the spin vector distribution of the main belt asteroids, not possible to explain by collisional factors. The spin vector evolution of the asteroids in the inner solar system, including the Earth- and Mars-crossing objects, is often subjected to strong forces related to frequencies in the orbital evolution. The variations in the spin vector direction are then very large and often subjected to chaos. The larger frequency related obliquity zones of the Mars-crossers are usually regular while the zones of the Earth-Mars-crossers often are of a chaotic nature. The spin vector evolution of asteroids with comet-like orbits is often chaotic regardless of initial obliquity. For the inner solar system asteroids, it is often possible for an initial prograde spin to turn into a retrograde one, or vice versa, due to the frequency related phenomena. Though some spin vector directions seem to be more probable than other ones over time, there are no indications for an evolution towards a more prograde or a more retrograde spin vector distribution.</p><p>The effects on the spin vector evolution from the thermal Yarkovsky force are examined for objects with radii larger than 50 m. This force will affect the orbital evolution and thus indirectly affect the spin vector evolution. However, it is found that the studied effects are minor as compared to the gravitationally related ones. This is true both for the diurnal and the seasonal variants of the Yarkovsky force.</p>

The dynamical evolution of the spin axis direction due to gravitational and thermal factors is examined. It is found that the spin axis variations generally are regular and relatively small for the bodies in the asteroid main belt. There are also reasons to believe that this is the case for minor objects beyond the main belt. However, it is found that these regular variations are larger when the orbital inclination of the objects is increased. This effect may explain certain features in the spin vector distribution of the main belt asteroids, not possible to explain by collisional factors. The spin vector evolution of the asteroids in the inner solar system, including the Earth- and Mars-crossing objects, is often subjected to strong forces related to frequencies in the orbital evolution. The variations in the spin vector direction are then very large and often subjected to chaos. The larger frequency related obliquity zones of the Mars-crossers are usually regular while the zones of the Earth-Mars-crossers often are of a chaotic nature. The spin vector evolution of asteroids with comet-like orbits is often chaotic regardless of initial obliquity. For the inner solar system asteroids, it is often possible for an initial prograde spin to turn into a retrograde one, or vice versa, due to the frequency related phenomena. Though some spin vector directions seem to be more probable than other ones over time, there are no indications for an evolution towards a more prograde or a more retrograde spin vector distribution. The effects on the spin vector evolution from the thermal Yarkovsky force are examined for objects with radii larger than 50 m. This force will affect the orbital evolution and thus indirectly affect the spin vector evolution. However, it is found that the studied effects are minor as compared to the gravitationally related ones. This is true both for the diurnal and the seasonal variants of the Yarkovsky force.