In this thesis, we study the influence of non-gravitational perturbations induced by the Yarkovsky/YORP effect and solar radiation pressure (SRP) on the orbital evolution of selected asteroids, asteroid families and pairs. These perturbations are of great importance if one wants to perform precise and long-term propagation of meter-sized and kilometer-sized bodies. Although they have found many applications in the Solar System, here, we particularly investigated how they influence the orbit of near-Earth asteroid (99942) Apophis and what is their role in the age determination of asteroid families and pairs. Our numerical simulations showed that the perturbations of Apophis' orbit caused by the SRP are orders of magnitude smaller than those produced by the Yarkovsky effect. The age determination of asteroid families and pairs was another pillar of this work. Over the past decade it turned out that the Yarkovsky effect must be taken into account for backward propagation of pair/family members. We modified the current method for estimating the age of asteroid pairs to be suitable for weakly convergent cases and discovered 7 young pairs with similar-sized components, which is in contradiction with the current theory of pair formation. In addition, we focused on an interesting pair of asteroids -...

Made available in DSpace on 2014-06-11T19:25:29Z (GMT). No. of bitstreams: 0 Previous issue date: 2011-05-27Bitstream added on 2014-06-13T20:33:08Z : No. of bitstreams: 1 boldrin_lag_me_guara.pdf: 3330498 bytes, checksum: 08e50694f19fe39f5f0bffa60c6c5946 (MD5) / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / A compreensão do universo é um dos grandes desejos da humanidade desde o princípio, e o estudo do movimento dos corpos celestes é uma parte deste todo. Dentro deste contexto está nosso trabalho, que tem como meta o estudo da dinâmica de asteróides múltiplos do nosso sistema solar, sendo este composto pelo movimento de translação dos asteróides satélites (asteróides menores que orbitam um de maior porte) e o movimento de atitude do asteróide central (asteróide de maior porte). O estudo dos asteróides múltiplos é uma grande chave para o conhecimento do passado de nosso sistema solar, visto que os mesmos são remanescentes da formação dos planetas. Partindo dessa motivação, realizamos um trabalho sobre a dinâmica do sistema (87) Sylvia no qual estudamos por meio de simulações numéricas a dinâmica dos satélites de Sylvia perturbados por Sol e Júpiter (Winter et al, 2009). Neste estudo foi mostrado que Rômulo e Remo sofrem fortes perturbações seculares provenientes de Sol e Júpiter, que poderiam desestabilizá-los. Descobrimos também que o achatamento (J2) do corpo central é de extrema importância na estabilidade dos satélites. Partindo desse resultado, para este trabalho, decidimos fazer uma análise mais minuciosa do problema em questão. Para isso, nós realizamos simulações considerando o movimento de atitude do asteróide central, algo até agora não considerado por nós. Este movimento de atitude é perturbado pelos torques causados por seus satélites, Sol e planetas. Apresentaremos neste trabalho uma sucinta abordagem teórica de nosso modelo juntamente com uma revisão bibliográfica de alguns modelos analítico aproximados encontrados na literatura, alguns testes de nossa ferramenta computacional e um estudo de dois sistemas triplos de asteróides conhecidos. Os sistemas estudados foram (87) Sylvia e (45) Eugenia. Os resultados nos mostrou que... / The understanding of the universe is one of the greats desires of humanity since the beginning, and the study of movement of celestial bodies is a part of it. Inside this context lies our work, which has as goal the study of the dynamics of multiple asteroids from our solar system, being this one compound of the movement of translation of the satellite asteroids (smaller asteroids which orbit one of larger size) and the movement of attitude of the central asteroid (largest size asteroid). The study of multiple asteroids is a great key for knowledge of our solar system past, since they are remaining objects of the formation of planets. Starting from that motivation, we developed a work about the dynamics of the system (87) Sylvia, in which we studied through numerical simulations the dynamics of Sylvia’s satellites perturbed by Sun and Jupiter (Winter et al, 2009). In this study, it has been shown that Romulus and Remus experience strong secular perturbations from Sun and Jupiter, which could destabilize them. We also found out that the flatness (J2) of the central body is of extreme importance in the stability of the satellites. Based on this result, for this work, we decided to do a closer analysis of the problem concerned. To do so, we developed simulations considering the movement of attitude of the central asteroid, which, so far, has not been considered by us. This movement of attitude is perturbed by torques caused by their satellites, Sun and planets. We will present in this work a brief theoretical approach of our model along with a bibliographic review of some approximate analytical models found in the literature, some tests of our computational tool and a study of two familiar triple systems of asteroids. The studied systems was (87) Sylvia and (45) Eugenia. The results has shown us that the movement of attitude of the central body experience great perturbation due to the Sun... (Complete abstract click electronic access below)

Orientador: Othon Cabo Winter / Co orientador: Rodney da Silva Gomes / Banca: Silvia Maria Giuliatti Winter / Banca: Nelson Callegari Junior / Resumo: A compreensão do universo é um dos grandes desejos da humanidade desde o princípio, e o estudo do movimento dos corpos celestes é uma parte deste todo. Dentro deste contexto está nosso trabalho, que tem como meta o estudo da dinâmica de asteróides múltiplos do nosso sistema solar, sendo este composto pelo movimento de translação dos asteróides satélites (asteróides menores que orbitam um de maior porte) e o movimento de atitude do asteróide central (asteróide de maior porte). O estudo dos asteróides múltiplos é uma grande chave para o conhecimento do passado de nosso sistema solar, visto que os mesmos são remanescentes da formação dos planetas. Partindo dessa motivação, realizamos um trabalho sobre a dinâmica do sistema (87) Sylvia no qual estudamos por meio de simulações numéricas a dinâmica dos satélites de Sylvia perturbados por Sol e Júpiter (Winter et al, 2009). Neste estudo foi mostrado que Rômulo e Remo sofrem fortes perturbações seculares provenientes de Sol e Júpiter, que poderiam desestabilizá-los. Descobrimos também que o achatamento (J2) do corpo central é de extrema importância na estabilidade dos satélites. Partindo desse resultado, para este trabalho, decidimos fazer uma análise mais minuciosa do problema em questão. Para isso, nós realizamos simulações considerando o movimento de atitude do asteróide central, algo até agora não considerado por nós. Este movimento de atitude é perturbado pelos torques causados por seus satélites, Sol e planetas. Apresentaremos neste trabalho uma sucinta abordagem teórica de nosso modelo juntamente com uma revisão bibliográfica de alguns modelos analítico aproximados encontrados na literatura, alguns testes de nossa ferramenta computacional e um estudo de dois sistemas triplos de asteróides conhecidos. Os sistemas estudados foram (87) Sylvia e (45) Eugenia. Os resultados nos mostrou que... (Resumo completo, clicar acesso eletrônico abaixo) / Abstract: The understanding of the universe is one of the greats desires of humanity since the beginning, and the study of movement of celestial bodies is a part of it. Inside this context lies our work, which has as goal the study of the dynamics of multiple asteroids from our solar system, being this one compound of the movement of translation of the satellite asteroids (smaller asteroids which orbit one of larger size) and the movement of attitude of the central asteroid (largest size asteroid). The study of multiple asteroids is a great key for knowledge of our solar system past, since they are remaining objects of the formation of planets. Starting from that motivation, we developed a work about the dynamics of the system (87) Sylvia, in which we studied through numerical simulations the dynamics of Sylvia's satellites perturbed by Sun and Jupiter (Winter et al, 2009). In this study, it has been shown that Romulus and Remus experience strong secular perturbations from Sun and Jupiter, which could destabilize them. We also found out that the flatness (J2) of the central body is of extreme importance in the stability of the satellites. Based on this result, for this work, we decided to do a closer analysis of the problem concerned. To do so, we developed simulations considering the movement of attitude of the central asteroid, which, so far, has not been considered by us. This movement of attitude is perturbed by torques caused by their satellites, Sun and planets. We will present in this work a brief theoretical approach of our model along with a bibliographic review of some approximate analytical models found in the literature, some tests of our computational tool and a study of two familiar triple systems of asteroids. The studied systems was (87) Sylvia and (45) Eugenia. The results has shown us that the movement of attitude of the central body experience great perturbation due to the Sun... (Complete abstract click electronic access below) / Mestre

In this thesis, I describe the main ideas and summarize the results of four refereed papers I contributed to (three times as the second author and once as the first author). The first step of each of these papers was the identification of genetically related asteroid and their membership confirmation. Since members of asteroid pairs and clusters have a very similar heliocentric orbits, we employed and further developed methods based on backward orbital integrations. The chronologically first paper Pravec et al. (2018) deals with asteroid clusters and their similarity to asteroid pairs. The second paper Pravec et al. (2019) is a complex study of 93 asteroid pairs with many interesting results, such as the existence of binary asteroids among asteroid pairs. The third paper Moskovitz et al. (2019) deals with an identification of asteroid pairs in the near-Earth population and a detail study of two probable asteroid pairs. The fourth paper, Fatka et al. (2020), studies the phenomenon of cascade disruption in asteroid clusters, which results in multiple generations (with different ages) of escaped secondaries in some asteroid clusters.

In this work, capturing Near-Earth Asteroids (NEAs) into Near-Earth orbits is investigated. A general optimization strategy is employed whereby a genetic algorithm is used to seed a sequential quadratic programming (SQP) method for the first step, and then nearby solutions seed further SQP runs. A large number of solutions are produced for several asteroids with varying levels of thrust, and under the effects of various perturbations. Solutions are found over a range of epochs and times of flight as opposed to many traditional methods of optimizing point solutions. This methodology proved effective, finding low-thrust capture solutions within 10% of the required Delta V for analytically estimated transfers, and matching results from other optimization programs such as MALTO. It is found that the effects of solar radiation pressure (SRP) and n-body effects do not have a significant impact on the optimized transfer costs, nor do the perturbations significantly affect the shapes and trends of the optimized solution space. <p><br></p> <p>These optimized results are then used to develop analytic models for both optimized transfer costs and flight times. These models are then used to estimate the transfer costs and flight times for all listed Near Earth Asteroids from the JPL Small Body Database. This analysis is then used to determine the nominal properties of potentially capturable asteroids. The characteristics are then related to a series of different asteroid transfer technologies, elucidating each technology's capabilities and potential capture targets. Finally, this analysis concludes with a brief roadmap of the major decisions mission designers should consider for future asteroid capture missions.</p>

京都大学 / 0048 / 新制・課程博士 / 博士(工学) / 甲第20375号 / 工博第4312号 / 新制||工||1668(附属図書館) / 京都大学大学院工学研究科電気工学専攻 / (主査)教授 山川 宏, 教授 引原 隆士, 准教授 海老原 祐輔 / 学位規則第4条第1項該当 / Doctor of Philosophy (Engineering) / Kyoto University / DFAM

International Telemetering Conference Proceedings / October 28-31, 1996 / Town and Country Hotel and Convention Center, San Diego, California / The Near Earth Asteroid Rendezvous (NEAR) satellite will travel to the asteroid 433 Eros, arriving there early in 1999, and orbit the asteroid for 1 year taking measurements that will map the surface features and determine its elemental composition. NEAR is the first satellite to use the rate-1/6 convolutional encoding on its telemetry downlink. Due to the scarcity and complexity of full decoders, APL designed and built a less capable but inexpensive version of the decoder for use in the integration, test, and prelaunch checkout of the rate-1/6 encoder. This paper describes the rationale for the design, how it works, and the features that are included.

abstract: Mathematical models are important tools for addressing problems that exceed experimental capabilities. In this work, I present ordinary and partial differential equation (ODE, PDE) models for two problems: Vicodin abuse and impact cratering. The prescription opioid Vicodin is the nation's most widely prescribed pain reliever. The majority of Vicodin abusers are first introduced via prescription, distinguishing it from other drugs in which the most common path to abuse begins with experimentation. I develop and analyze two mathematical models of Vicodin use and abuse, considering only those patients with an initial Vicodin prescription. Through adjoint sensitivity analysis, I show that focusing efforts on prevention rather than treatment has greater success at reducing the total population of abusers. I prove that solutions to each model exist, are unique, and are non-negative. I also derive conditions for which these solutions are asymptotically stable. Verification and Validation (V&V) are necessary processes to ensure accuracy of computational methods. Simulations are essential for addressing impact cratering problems, because these problems often exceed experimental capabilities. I show that the Free Lagrange (FLAG) hydrocode, developed and maintained by Los Alamos National Laboratory, can be used for impact cratering simulations by verifying FLAG against two analytical models of aluminum-on-aluminum impacts at different impact velocities and validating FLAG against a glass-into-water laboratory impact experiment. My verification results show good agreement with the theoretical maximum pressures, and my mesh resolution study shows that FLAG converges at resolutions low enough to reduce the required computation time from about 28 hours to about 25 minutes. Asteroid 16 Psyche is the largest M-type (metallic) asteroid in the Main Asteroid Belt. Radar albedo data indicate Psyche's surface is rich in metallic content, but estimates for Psyche's composition vary widely. Psyche has two large impact structures in its Southern hemisphere, with estimated diameters from 50 km to 70 km and estimated depths up to 6.4 km. I use the FLAG hydrocode to model the formation of the largest of these impact structures. My results indicate an oblique angle of impact rather than a vertical impact. These results also support previous claims that Psyche is metallic and porous. / Dissertation/Thesis / Psyche asteroid impact simulation initialization / Psyche asteroid impact simulation video / Doctoral Dissertation Applied Mathematics 2019

CubeSats are becoming a game changer in the space industry. Appearing first for univer-sity mission, its popularity is increasing for commercial use and for deep space missionssuch as the on HERA mission that will orbit in 2026 around an asteroid as part of aplanetary defence mission. Standardisation and industrial collaboration is key to a fastdevelopment, assuring the product quality and lower development expenditures.In this study the focus is set elaborating a low cost demonstrator platform to be usedfor developing and testing onboard software on physical hardware: a Hardware-Softwaretesting facility. The purpose of such a platform is to create an interactive and accessibleenvironment for developing on board software. The application chosen to be elaboratedon this platform is a module the subsystem of attitude and orbit control of the satelliteorbiting around asteroid.In order to create this platform the simulation of the asteroid environment of theCubeSat has been made using open source software libraries. During this task the per-formance of open source libraries has been compared to commercial alternatives. In thedevelopment of simulation different orbit perturbations have been studied by modellingthe asteroid as a cube or spheroid and additionally the effect of a third perturbing bodyand radiation pressure.As part of this project two microcontroller have been set up communicating using acommunication bus and communication protocols used for space applications to simulatehow the attitude and orbit control is commanded inside the CubeSat.

In public opinion, protection against asteroids impact has always been on the agenda of space engineering. Actually it started from 1994 when Shoemaker Levy stroke Jupiter. This protection works in two steps: detection of threat and deflection. Some space agencies and foundations monitor the sky and set up scenario. Although the sky is nowadays well monitored and mapped, there is no global plan nowadays against this threat. This paper focuses on the deflection step, and aims at forecasting which variables are involved and their consequences on the deflection mission. In fact the result depends on several factors, like the time before hazardous moment, the accuracy of detection tools, the choice of deflection method, but the most unpredictable are human factors. This study shows a strategy and so tries to give some new response parts to the global deflection problem.