62 results on '"Gomes, Rodney"'
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52. Conveyed to the Kuiper belt
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Gomes, Rodney, primary
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- 2003
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53. A Global Study of the 3[rcolon]1 Resonance Neighborhood: A Search for Unstable Asteroids
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Guillens, Sueli A., primary, Vieira Martins, Roberto, additional, and Gomes, Rodney S., additional
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- 2002
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54. A numerical analysis of the process of capture into resonance
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Gomes, Rodney S., primary and Miguelote, Alexandre Y., additional
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- 1996
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55. Trapping of Dust Particles into Internal Resonances with the Inner Planets
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Gomes, Rodney S., primary
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- 1996
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56. The origin of TNO 2004 XR190 as a primordial scattered object
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Gomes, Rodney S.
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TRANS-Neptunian objects , *NUMERICAL integration , *DISKS (Astrophysics) , *SCATTERING (Physics) , *PLANETARY orbits , *KUIPER belt , *NEPTUNE (Planet) - Abstract
Abstract: Numerical integrations of the equations of motion of the giant planets and scattering particles show that there is a possible orbital itinerary that a particle may follow from a scattering mode up to a stable position near the orbit of 2004 XR190. This orbital evolution requires that the particle gets trapped in a mean motion resonance with Neptune coupled with the Kozai resonance. Imposing migration on Neptune while a particle is experiencing both resonances can entail an escape from resonance at a low particle’s eccentricity. This eccentricity and the associated inclination are always similar to those of 2004 XR190. I conclude that 2004 XR190 was most likely a scattered object that went through those resonance processes and was eventually deposited at its current position. By the same argument, it is expected that there must exist several other objects with similar semimajor axis, eccentricity and inclination as those of 2004 XR190. [Copyright &y& Elsevier]
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- 2011
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57. Dynamical structure and origin of the Trans-Neptunian population.
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Gomes, Rodney S.
- Abstract
Before the discovery of the first member of the Kuiper belt in 1992, the trans-Neptunian population was supposed to lie on a flat disk and each member would follow a barely eccentric orbit. While less conventional orbits for the trans-Neptunian objects were being discovered, our understanding of its orbital structure and origin was continually changed. A basic classification of the trans-Neptunian population as to their orbits identifies a classical low inclination Kuiper belt population, a resonant population, a high inclination Kuiper belt population, a scattered population and an extended population. Several mechanisms have been proposed to explain the orbital architecture of the Kuiper belt population. Presently, the most plausible scenarios are unequivocally related with the primordial planetary migration induced by a planetesimal disk. Low inclination orbits in the Kuiper belt may have been moderately pushed out from a dynamically cold primordial disk by the resonance sweeping mechanism. The origin of high inclination objects in the classical Kuiper belt is however to be found in a primordial Neptune scattered population, through a perihelion increasing mechanism based on secular resonances. Another push-out mechanism based on the sweeping of the 1:2 resonance with Neptune has also been invoked to explain the low inclination orbits in the classical Kuiper belt. Assuming these last two mechanisms, Kuiper belt objects do not need to have been formed in situ. This kind of formation process would demand a quite large original mass in the Kuiper belt region, which would have brought Neptune beyond its present position at 30 AU. Thus with the exception of the low inclination classical Kuiper belt objects and a few resonant ones, all other trans-Neptunian objects are present or past scattered objects. This notion also includes the case for Sedna, so far the only certain member of the extended population. In its most plausible formation scenario, it was a primordial scattered object by Neptune whose perihelion was increased by the close passage of a star. [ABSTRACT FROM PUBLISHER]
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- 2005
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58. Validation of Sagnier's theory by its application to the major planets.
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Silva Gomes, Rodney
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In this paper, the theory of Sagnier was applied to the major planets, in order to have a first evaluation of this theory which was built, primarily, to study the galilean satellites of Jupiter. In this application we included the first order of the intermediary solution and the solution of the linear variational equations. Results from other theories, mainly those of Simon and Bretagnon, have been used as basis for comparisons. The results and their comparisons are shown by means of tables of coefficients and proper frequencies and graphs of variations of the orbital elements. [ABSTRACT FROM AUTHOR]
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- 1986
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59. Exciting an Initially Cold Asteroid Belt Through a Planetary Instability
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Deienno, Rogerio, Izidoro, A., Morbidelli, Alessandro, Gomes, Rodney, Nesvorny, David, Raymond, Sean N., Universidade Estadual Paulista Júlio de Mesquita Filho [São José do Rio Preto] ( UNESP ), Universidade Estadual Paulista Júlio de Mesquita Filho, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides ( CASSIOPEE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Space Studies [Boulder], Southwest Research Institute [Boulder] ( SwRI ), ECLIPSE 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Universidade Estadual Paulista Júlio de Mesquita Filho = São Paulo State University (UNESP), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Southwest Research Institute [Boulder] (SwRI), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
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[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,Astrophysics::Earth and Planetary Astrophysics ,[ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] - Abstract
International audience; The main asteroid belt (MB) is low in mass but dynamically excited, with much larger eccentricities and inclinations than the planets. In recent years, the Grand Tack model has been the predominant model capable of reconciling the formation of the terrestrial planets with a depleted but excited MB. Despite this success, the Grand Tack is still not generally accepted because of uncertainties in orbital migration. It was recently proposed that chaotic early evolution of Jupiter and Saturn could excite the initially cold MB. However, hydrodynamical simulations predict that the giant planets should generally emerge from the gas disk phase on orbits characterized by resonant and regular motion. Here we propose a new mechanism to excite the MB during the giant planets' ('Nice model') instability, which is expected to have included repeated close encounters between Jupiter and one or more ice giants ('Jumping Jupiter' -- JJ). We show that when Jupiter temporarily reaches a high enough level of excitation, both in eccentricity and inclination, it induces strong forced vectors of eccentricity and inclination within the MB region. Because during the JJ instability Jupiter's orbit 'jumps' around, forced vectors keep changing both in magnitude and phase throughout the whole MB region. The entire cold primordial MB can thus be excited as a natural outcome of the JJ instability. Furthermore, we show that the subsequent evolution of the Solar System is capable of reshaping the resultant MB to its present day orbital state, and that a strong mass depletion is always associated to the JJ instability phase.
60. LATE ORBITAL INSTABILITIES IN THE OUTER PLANETS INDUCED BY INTERACTION WITH A SELF-GRAVITATING PLANETESIMAL DISK
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Gomes, Rodney [Observatorio Nacional/MCT, Rio de Janeiro, RJ (Brazil)]
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- 2011
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61. The instability in the dynamical evolution of the solar system: sonsiderations about the time of instability and formation of the Kuiper belt
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Sousa, Rafael Ribeiro de, Universidade Estadual Paulista (Unesp), Vieira Neto, Ernesto [UNESP], Gomes, Rodney da Silva [UNESP], and Morbidelli, Alessandro
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Disco de Planetesimais ,Cinturão de Kuiper ,Solar System formation ,giant planet instability ,Formação do Sistema Solar ,Astronomia ,Kuiper Belt ,Dinâmica Secular ,Instabilidade Planetária ,Sistema Solar ,Planetesimal disk ,Secular dynamics - Abstract
Submitted by Rafael Ribeiro De Sousa (r.sousa@unesp.br) on 2019-09-10T15:28:55Z No. of bitstreams: 1 Versao_Final_RafaelRibeiro_Doutorado.pdf: 80337347 bytes, checksum: 22905a7f9a40edc10c7054045e1d2b9a (MD5) Approved for entry into archive by Pamella Benevides Gonçalves null (pamella@feg.unesp.br) on 2019-09-11T19:46:57Z (GMT) No. of bitstreams: 1 sousa_rr_dr_guara_par.pdf: 2999056 bytes, checksum: f4b99a74e0617478acbfb4dee1de9ec5 (MD5) Made available in DSpace on 2019-09-11T19:46:57Z (GMT). No. of bitstreams: 1 sousa_rr_dr_guara_par.pdf: 2999056 bytes, checksum: f4b99a74e0617478acbfb4dee1de9ec5 (MD5) Previous issue date: 2019-09-05 Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) O estudo da formação e evolução do Sistema Solar é uma fonte de informação para entender sob quais condições a vida poderia surgir e evoluir. Nós apresentamos, nesta Tese de doutorado, um estudo numérico da fase final de acresção dos planetas gigantes do Sistema Solar durante e após a fase do disco de gás protoplanetário. Em nossas simulações, utilizamos um modelo recente e confiável para a formação de Urano e Netuno para esculpir as propriedades do disco trans-Netuniano original (Izidoro et al. , 2015a). Nós fizemos este estudo de uma maneira autoconsistente considerando os efeitos do gás e da evolução dos embriões planetários que formam Urano e Netuno por colisões gigantescas. Consideramos diferentes histórias de migração de Júpiter, devido a incerteza de como Júpiter migrou, durante a fase de gás. As nossas simulações permitiram obter pela primeira vez as propriedades orbitais do disco trans-Netuniano original. Então, calculamos o tempo de instabilidade dos planetas gigantes a partir de sistemas planetários que formam similares Urano e Netuno. Nossos resultados indicam fortemente que a instabilidade dos planetas gigantes acontecem cedo em até 500 milhões de anos e mais provável ainda ter acontecido em 136 milhões de anos após a dissipação do gás. Nós também realizamos simulações para discutir alguns efeitos dinâmicos que acontecem na região do cinturão de Kuiper. Estes efeitos acontecem quando Netuno esteve em alta excentricidade durante a instabilidade planetária. Para este problema, usamos as simulações realizadas por Gomes et al. (2018) que investigaram a compatibilidade da formação do cinturão frio de Kuiper, no referencial mais recente do modelo de Nice. A produção da população fria acontece in situ em Gomes et al. (2018) com o disco de planetesimais estendido até 45 ua. As simulações de Gomes et al. (2018) apresentaram bons resultados mas algumas evoluções de Netuno são muito drásticas para obter excentricidades baixas compatíveis as quais estão presentes no atual cinturão de Kuiper. Nós realizamos simulações para a produção da população fria diante de uma fase que é mais prejudicial para a retenção dessa população: a fase excêntrica de Netuno (e > 0.2) e a precessão lenta da longitude do periélio deste planeta (Batygin et al. , 2011). Refizemos estas simulações considerando agora a interação mútua de objetos com tamanho de alguns plutões, ou menores, embutidos no cinturão de Kuiper. Com estes resultados, podemos verificar se a dispersão causada pela autogravidade é capaz de produzir objetos com excentricidade mais baixas durante a fase violenta de Netuno. Nós também aplicamos a teoria secular para explicar os nossos resultados. Obtermos excentricidades baixas com a autogravidade dos planetesimais mas considerando um disco mais massivo do que é observado no cinturão frio de Kuiper. Portanto, concluímos que o ingrediente principal para a retenção da população fria, quando Netuno estava em alta excentricidade, é um sincronismo entre a duração dos ciclos seculares e o fim da fase de precessão lenta de Netuno. A study of the formation and evolution of the Solar System is a source of information for an understanding of what conditions life could arise and evolve. We present a numerical study of the final stage of accretion of the giant planets of the Solar System during and after the protoplanetary gas disc phase. In our simulations, we use a recent and reliable model for the formation of Uranus and Neptune to sculpt the properties of the original trans-Neptunian disk (Izidoro et al. , 2015a). We have done this study in a self-consistent way considering the effects of gas and the evolution of planetary embryos which form Uranus and Neptune by mutual giant collisions. We considered different Jupiter migration stories due to the uncertainty of how Jupiter’s migration was during the gas phase. Our simulations provide for the first time to obtain the orbital properties of the original trans-Neptunian disk. We then calculate the instability time of the giant planets from planetary systems which form similar Uranus and Neptune. Our results strongly indicate that the instability of the giant planets occurs early within 500 million years and even more likely to happen at 136 million years after gas dissipation. We also perform simulations to discuss some dynamical effects that happen in the Kuiper belt region. These effects happen when Neptune was in high eccentricity during planetary instability. For this problem, we use the simulations performed by Gomes et al. (2018) who investigated the compatibility of the Kuiper cold belt formation in the latest Nice model framework. Cold population production takes place in situ in Gomes et al. (2018) with planetesimal disc extended to 45 AU. The simulations of Gomes et al. (2018) have shown good results but some Neptune evolutions are too drastic to obtain low eccentricities which are present in the current Kuiper belt. We perform simulations for the production of the cold population in the face of a phase that is most drastic for the cold population’s retention: the eccentric phase of Neptune (e > 0.2) and the slow precession of the perihelion longitude of this planet (Batygin et al. , 2011). We performed new simulations but considering the mutual interaction of objects (self-gravity) with the size of a few pluto, or smaller, embedded in the Kuiper belt. With these results, we can see if the dispersion caused by the self-gravity is capable of producing lower eccentricity objects during the violent phase of Neptune. We also apply secular theory to explain our results. The planetesimals reach low eccentricities with the self-gravity but considering a more massive disk than the observed Kuiper belt. Therefore, we conclude that the ideal for Neptune’s evolution to produce the cold population even at high eccentricity is the synchronism between the secular cycles of the planetesimals and the duration of Neptune’s eccentric and slow precession phase. FAPESP: 2015/15588-9 FAPESP: 2017/09919-8 FAPESP: 2016/24561-0 CAPES: 001
- Published
- 2019
62. Dinâmica do sistema binário Plutão-Caronte
- Author
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Santos, Pryscilla Maria Pires dos [UNESP], Universidade Estadual Paulista (Unesp), and Gomes, Rodney da Silva [UNESP]
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Sistema solar ,Plutão (Planeta) ,Estrelas binárias ,Planetas - Orbitas ,Satelites ,Pluto (Planet) ,Metodos de simulação - Abstract
Made available in DSpace on 2014-12-02T11:16:54Z (GMT). No. of bitstreams: 0 Previous issue date: 2014-03-20Bitstream added on 2014-12-02T11:20:56Z : No. of bitstreams: 1 000791753.pdf: 2751318 bytes, checksum: 273e7cbadcaa9ed81c675b41ad4a9fb7 (MD5) Neste trabalho investigamos a evolução orbital de partículas de poeira que escapam das superfícies de ambos satélites pequenos de Plutão: Nix e Hidra, produzidas através do impacto de micrometeoroides nas superfícies dos mesmos, sob influencia da pressão de radiação solar e dos efeitos gravitacionais de Plutão, Caronte e dos próprios satélites fontes (Nix e Hidra). A taxa de produção de massa dos grãos de poeira micrométricos foi obtida e simulações numéricas foram realizadas para obter o tempo de vida destes grãos no sistema plutoniano. Os grãos ejetados de Nix e Hidra formam um anel de largura de aproximadamente 16.000 km, o que corresponde a distância radial aproximada entre as órbitas de Nix e Hidra. Através das integrações numéricas verificamos que colisões de grãos com os corpos massivos do sistema e escape em _orbitas hiperbólicas constituem os principais mecanismos de perda de material e são determinadas pelo efeito da pressão de radiação solar. Este importante mecanismo de desestabilização de grãos de poeira em Plutão, remove 30% do conjunto inicial de partículas com raios de 1 µ em apenas 1 ano. As demais partículas que permanecem no sistema formam um anel muito tênue com uma profundidade óptica máxima de 4x10¹¹. Exploramos também a possibilidade dos progenitores dos satélites pequenos de Plutão terem sido capturados pelo binário Plutão-Caronte do disco primordial massivo heliocêntrico, no qual Plutão estaria inserido. Encontramos que, para objetos com baixas velocidades de aproximação com o binário, capturas poderiam ocorrer com probabilidade não é negligenciável devido a natureza do próprio encontro: planetesimal e par de objetos massivosNo entanto, os objetos capturados permaneceriam em orbitas bastante excêntricas em relação ao baricentro do binário, assim o tempo tópico de ... (Resumo completo, clicar acesso eletrônico abaixo) In this work, we investigate the orbital evolution of the escaping dust from both small satellites of Pluto: Nix and Hydra, produced via impacts of micrometeoroids on the surfaces of the small satellites, under the influence of the solar radiation pressure combined with the gravitational ejects of Pluto, Charon, and the parent-bodies (Nix and Hydra). The mass production rate of micron-sized dust particles is obtained and numerical simulations are performed to derive the lifetime of the ejecta. The ejected particles form a wide ring of about 16,000 km, which corresponds to the radial distance between the orbits of Nix and Hydra. Through the numerical simulations we verified that collisions with the massive bodies within the system and escape into hyperbolic orbits are the main mechanisms of loss of material, which are mainly determined by the solar radiation pressure acting on the grains. This important loss mechanism removes 30% of the initial set of 1 µ sized particles in 1 year. The surviving particles form a ring too faint to be detectable with a derived maximum optical depth of 4x10¹¹. We also explore the possibility that the progenitors of the small satellites of Pluto have been captured by the Pluto-Charon binary from the massive heliocentric planetesimal disk in which Pluto was originally embedded into. Wend that debris with small approximation velocities to the binary can be captured temporarily by Pluto-Charon with non-negligible probability, due to the dynamical perturbations exerted by the binary nature of the Pluto-Charon pair... (Complete abstract click eletronic access below)
- Published
- 2014
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