15 results on '"Gomes, Rodney"'
Search Results
2. On the origin of the Kuiper belt
- Author
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Gomes, Rodney da Silva
- Published
- 2009
- Full Text
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3. The Common Origin of the High Inclination TNO's
- Author
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Gomes, Rodney
- Published
- 2003
- Full Text
- View/download PDF
4. Dynamical effects on the classical Kuiper belt during the excited-Neptune model.
- Author
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Ribeiro de Sousa, Rafael, Gomes, Rodney, Morbidelli, Alessandro, and Vieira Neto, Ernesto
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KUIPER belt , *SOLAR system , *GAS giants , *PLANETESIMALS , *PLUTO (Dwarf planet) , *TIME measurements - Abstract
• Simulations with an excited Neptune overexcite the KB cold population. • A self graviting planetesimal disk helps objects to return to an unexcited mode. • The self-gravity is effective just for a cold population with Pluto-sized objects. • Without self gravity, we need very specific secular configurations for Neptune. The link between the dynamical evolution of the giant planets and the Kuiper Belt orbital structure can provide clues and insight about the dynamical history of the Solar System. The classical region of the Kuiper Belt has two populations (the cold and hot populations) with completely different physical and dynamical properties. These properties have been explained in the framework of a sub-set of the simulations of the Nice Model , in which Neptune remained on a low-eccentricity orbit (Neptune's eccentricity is never larger than 0.1) throughout the giant planet instability (Nesvorný 2015a,b). However, recent simulations (Gomes et al., 2018) have showed that the remaining Nice model simulations, in which Neptune temporarily acquires a large-eccentricity orbit (larger than 0.1), are also consistent with the preservation of the cold population (inclination smaller than 4°), if the latter formed in situ. However, the resulting a cold population showed in many of the simulations eccentricities larger than those observed for the real population. The purpose of this work is to discuss the dynamical effects on the Kuiper belt region due to an excited Neptune phase. We focus on a short period of time, of about six hundred thousand years, which is characterized by Neptune's large eccentricity and smooth migration with a slow precession of Neptune's perihelion. This phase was observed during a full simulation of the Nice Model (Gomes et al., 2018) just after the last jump of Neptune's orbit due to an encounter with another planet. We show that if self-gravity is considered in the disk, the precession rate of the particles longitude of perihelion ϖ is slowed down, which in turn speeds up the cycle of ϖ N − ϖ (the subscript N referring to Neptune), associated to the particles eccentricity evolution. This, combined with the effect of mutual scattering among the bodies, which spreads all orbital elements, allows some objects to return to low eccentricities. However, we show that if the cold population originally had a small total mass, this effect is negligible. Thus, we conclude that the only possibilities to keep at low eccentricity some cold-population objects during a high-eccentricity phase of Neptune are that (i) either Neptune's precession was rapid, as suggested by Batygin et al. (2011) or (ii) Neptune's slow precession phase was long enough to allow some particles to experience a full secular cycle of ϖ − ϖ N. [ABSTRACT FROM AUTHOR]
- Published
- 2019
- Full Text
- View/download PDF
5. Checking the compatibility of the cold Kuiper belt with a planetary instability migration model.
- Author
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Gomes, Rodney, Nesvorný, David, Morbidelli, Alessandro, Deienno, Rogerio, and Nogueira, Erica
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KUIPER belt , *PLANETARY systems , *SIMULATION methods & models , *DEFORMATIONS (Mechanics) , *STRUCTURAL dynamics - Abstract
The origin of the orbital structure of the cold component of the Kuiper belt is still a hot subject of investigation. Several features of the solar system suggest that the giant planets underwent a phase of global dynamical instability, but the actual dynamical evolution of the planets during the instability is still debated. To explain the structure of the cold Kuiper belt, Nesvorny (2015, AJ 150,68) argued for a ”soft” instability, during which Neptune never achieved a very eccentric orbit. Here we investigate the possibility of a more violent instability, from an initially more compact fully resonant configuration of 5 giant planets. We show that the orbital structure of the cold Kuiper belt can be reproduced quite well provided that the cold population formed in situ, with an outer edge between 44 − 45 au and never had a large mass. [ABSTRACT FROM AUTHOR]
- Published
- 2018
- Full Text
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6. The origin of TNO 2004 XR190 as a primordial scattered object
- Author
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Gomes, Rodney S.
- Subjects
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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]
- Published
- 2011
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7. A distant planetary-mass solar companion may have produced distant detached objects
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Gomes, Rodney S., Matese, John J., and Lissauer, Jack J.
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ASTRONOMICAL perturbation , *PLANETS , *KUIPER belt , *SOLAR system - Abstract
Abstract: Most known trans-neptunian objects (TNO''s) are either on low eccentricity orbits or could have been perturbed to their current trajectories via gravitational interactions with known bodies. However, one or two recently-discovered TNO''s are distant detached objects (DDO''s) (perihelion, and semimajor axis, ) whose origins are not as easily understood. We investigate the parameter space of a hypothetical distant planetary-mass solar companion which could detach the perihelion of a Neptune-dominated TNO into a DDO orbit. Perturbations of the giant planets are also included. The problem is analyzed using two models. In the first model, we start with a distribution of undetached, low-inclination TNO''s having a wide range of semimajor axes. The planetary perturbations and the companion perturbation are treated in the adiabatic, secularly averaged tidal approximation. This provides a starting point for a more detailed analysis by providing insights as to the companion parameter space likely to create DDO''s. The second model includes the companion and the planets and numerically integrates perturbations on a sampling that is based on the real population of scattered disk objects (SDO''s). A single calculation is performed including the mutual interactions and migration of the planets. By comparing these models, we distinguish the distant detached population that can be attributable to the secular interaction from those that require additional planetary perturbations. We find that a DDO can be produced by a hypothetical Neptune-mass companion having semiminor axis, or a Jupiter-mass companion with . DDO''s produced by such a companion are likely to have small inclinations to the ecliptic only if the companion''s orbit is significantly inclined. We also discuss the possibility that the tilt of the planets'' invariable plane relative to the solar equatorial plane has been produced by such a hypothetical distant planetary-mass companion. Perturbations of a companion on Oort cloud comets are also considered. [Copyright &y& Elsevier]
- Published
- 2006
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8. Dynamical structure and origin of the Trans-Neptunian population.
- Author
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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]
- Published
- 2005
- Full Text
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9. Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU?
- Author
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Gomes, Rodney S., Morbidelli, Alessandro, and Levison, Harold F.
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NEPTUNE (Planet) , *KUIPER belt , *EARTH (Planet) , *SOLAR system - Abstract
We study planetary migration in a gas-free disk of planetesimals. In the case of our Solar System we show that Neptune could have had either a damped migration, limited to a few AUs, or a forced migration up to the disk''s edge, depending on the disk''s mass density. We also study the possibility of runaway migration of isolated planets in very massive disk, which might be relevant for extra-solar systems. We investigate the problem of the mass depletion of the Kuiper belt in the light of planetary migration and conclude that the belt lost its pristine mass well before that Neptune reached its current position. Therefore, Neptune effectively hit the outer edge of the proto-planetary disk. We also investigate the dynamics of massive planetary embryos embedded in the planetesimal disk. We conclude that the elimination of Earth-mass or Mars-mass embryos originally placed outside the initial location of Neptune also requires the existence of a disk edge near
30 AU. [Copyright &y& Elsevier]- Published
- 2004
- Full Text
- View/download PDF
10. The origin of the Kuiper Belt high–inclination population
- Author
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Gomes, Rodney S.
- Subjects
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KUIPER belt , *RESONANCE - Abstract
I simulate the orbital evolution of the four major planets and a massive primordial planetesimal disk composed of 104 objects, which perturb the planets but not themselves. As Neptune migrates by energy and angular momentum exchange with the planetesimals, a large number of primordial Neptune-scattered objects are formed. These objects may experience secular, Kozai, and mean motion resonances that induce temporary decrease of their eccentricities. Because planets are migrating, some planetesimals can escape those resonances while in a low-eccentricity incursion, thus avoiding the return path to Neptune close encounter dynamics. In the end, this mechanism produces stable orbits with high inclination and moderate eccentricities. The population so formed together with the objects coming from the classical resonance sweeping process, originates a bimodal distribution for the Kuiper Belt orbits. The inclinations obtained by the simulations can attain values above 30° and their distribution resembles a debiased distribution for the high-inclination population coming from the real classical Kuiper Belt. [Copyright &y& Elsevier]
- Published
- 2003
- Full Text
- View/download PDF
11. The formation of the cold classical Kuiper Belt by a short range transport mechanism.
- Author
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Gomes, Rodney
- Subjects
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KUIPER belt , *PLANETESIMALS , *SOLAR system , *PEBBLES , *SPACE exploration - Abstract
The Classical Kuiper Belt is populated by a group of objects with low inclination orbits, reddish colors and usually belonging to a binary system. This so called Cold Classical Kuiper Belt is considered to have been formed in situ from primordial ice pebbles that coagulated into planetesimals hundreds of kilometers in diameter. According to this scenario, the accretion of pebbles into large planetesimals would have occurred through the streaming instability mechanism that would be effective in the primordial Solar System disk of gas and solids. Nevertheless other objects with the same color characteristics as those found in the Cold Classical Kuiper Belt can be encountered also past the 2:1 mean motion resonance with Neptune as scattered or detached objects. Here I propose a mechanism that can account for both the cold Classical Kuiper Belt objects and other reddish objects outside the Classical Kuiper Belt. According to the proposed scenario, reddish objects were primordially in the outer portion of the planetesimal disk which was however truncated somewhere below ~42 au. In this manner the cold Classical Kuiper Belt and its scattered / detached counterpart were respectively transported outwards by a short range or slightly scattered to their present locations. Resonant objects were also formed by the same process. This mechanism is aimed at explaining the distribution of all objects that share the same color characteristics as coming from a common origin in the outer borders of the primordial planetesimal disk. According to the scenario here proposed the Cold Classical Kuiper Belt would have been formed ~4 au inside its present location with a total mass 20 − 100 times as large as its present value. • The Cold Classical Kuiper Belt is usually believed to be formed in situ. • I propose a scenario by which the CCKB was transported a short distance from the planetesimal disk. • This scenario can account for the implantation of reddish objects as detached and resonant TNOs. • In this scenario the cold KB objects would be formed with a mass 20 to 100 times as large as the present CCKB. [ABSTRACT FROM AUTHOR]
- Published
- 2021
- Full Text
- View/download PDF
12. Planetary science: Conveyed to the Kuiper belt.
- Author
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Gomes, Rodney
- Subjects
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KUIPER belt , *SUN , *SOLAR system , *MASS (Physics) , *DUST , *SOLAR cycle - Abstract
The small icy bodies that make up the Kuiper belt are the most distant objects known in the Solar System. It also suggests that these objects formed much closer to the Sun since the first member of the Kuiper belt was discovered in 1992. Many unexpected features of their orbits and physical properties have been uncovered. It was predicted to be a hundred times larger than the mass of the Earth. To explain the missing mass, it has been proposed that collisions between Kuiper-belt objects over the lifetime of the Solar System have gradually transformed most of their mass into dust.
- Published
- 2003
- Full Text
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13. Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune
- Author
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Levison, Harold F., Morbidelli, Alessandro, VanLaerhoven, Christa, Gomes, Rodney, and Tsiganis, Kleomenis
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ASTRONOMY , *KUIPER belt , *URANUS (Planet) , *NEPTUNE (Planet) - Abstract
Abstract: We explore the origin and orbital evolution of the Kuiper belt in the framework of a recent model of the dynamical evolution of the giant planets, sometimes known as the Nice model. This model is characterized by a short, but violent, instability phase, during which the planets were on large eccentricity orbits. It successfully explains, for the first time, the current orbital architecture of the giant planets [Tsiganis, K., Gomes, R., Morbidelli, A., Levison, H.F., 2005. Nature 435, 459–461], the existence of the Trojans populations of Jupiter and Neptune [Morbidelli, A., Levison, H.F., Tsiganis, K., Gomes, R., 2005. Nature 435, 462–465], and the origin of the late heavy bombardment of the terrestrial planets [Gomes, R., Levison, H.F., Tsiganis, K., Morbidelli, A., 2005. Nature 435, 466–469]. One characteristic of this model is that the proto-planetary disk must have been truncated at roughly 30 to so that Neptune would stop migrating at its currently observed location. As a result, the Kuiper belt would have initially been empty. In this paper we present a new dynamical mechanism which can deliver objects from the region interior to to the Kuiper belt without excessive inclination excitation. In particular, we show that during the phase when Neptune''s eccentricity is large, the region interior to its 1:2 mean motion resonance becomes unstable and disk particles can diffuse into this area. In addition, we perform numerical simulations where the planets are forced to evolve using fictitious analytic forces, in a way consistent with the direct N-body simulations of the Nice model. Assuming that the last encounter with Uranus delivered Neptune onto a low-inclination orbit with a semi-major axis of and an eccentricity of ∼0.3, and that subsequently Neptune''s eccentricity damped in ∼1 My, our simulations reproduce the main observed properties of the Kuiper belt at an unprecedented level. In particular, our results explain, at least qualitatively: (1) the co-existence of resonant and non-resonant populations, (2) the eccentricity–inclination distribution of the Plutinos, (3) the peculiar semi-major axis—eccentricity distribution in the classical belt, (4) the outer edge at the 1:2 mean motion resonance with Neptune, (5) the bi-modal inclination distribution of the classical population, (6) the correlations between inclination and physical properties in the classical Kuiper belt, and (7) the existence of the so-called extended scattered disk. Nevertheless, we observe in the simulations a deficit of nearly-circular objects in the classical Kuiper belt. [Copyright &y& Elsevier]
- Published
- 2008
- Full Text
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14. The instability in the dynamical evolution of the solar system: sonsiderations about the time of instability and formation of the Kuiper belt
- Author
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Sousa, Rafael Ribeiro de, Universidade Estadual Paulista (Unesp), Vieira Neto, Ernesto [UNESP], Gomes, Rodney da Silva [UNESP], and Morbidelli, Alessandro
- Subjects
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
15. Dynamical evidence for an early giant planet instability.
- Author
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Ribeiro, Rafael de Sousa, Morbidelli, Alessandro, Raymond, Sean N., Izidoro, Andre, Gomes, Rodney, and Vieira Neto, Ernesto
- Subjects
- *
GAS giants , *SOLAR system , *KUIPER belt , *PLANETESIMALS , *PLANETARY systems , *JUPITER (Planet) , *ACCRETION disks - Abstract
The dynamical structure of the Solar System can be explained by a period of orbital instability experienced by the giant planets. While a late instability was originally proposed to explain the Late Heavy Bombardment, recent work favors an early instability. Here we model the early dynamical evolution of the outer Solar System to self-consistently constrain the most likely timing of the instability. We first simulate the dynamical sculpting of the primordial outer planetesimal disk during the accretion of Uranus and Neptune from migrating planetary embryos during the gas disk phase, and determine the separation between Neptune and the inner edge of the planetesimal disk. We performed simulations with a range of (inward and outward) migration histories for Jupiter. We find that, unless Jupiter migrated inwards by 10 AU or more, the instability almost certainly happened within 100 Myr of the start of Solar System formation. There are two distinct possible instability triggers. The first is an instability that is triggered by the planets themselves, with no appreciable influence from the planetesimal disk. About half of the planetary systems that we consider have a self-triggered instability. Of those, the median instability time is ∼ 4Myr. Among self-stable systems – where the planets are locked in a resonant chain that remains stable in the absence of a planetesimal's disk– our self-consistently sculpted planetesimal disks nonetheless trigger a giant planet instability with a median instability time of 37–62 Myr for a reasonable range of migration histories of Jupiter. The simulations that give the latest instability times are those that invoked long-range inward migration of Jupiter from 15 AU or beyond; however these simulations over-excited the inclinations of Kuiper belt objects and are inconsistent with the present-day Solar System. We conclude on dynamical grounds that the giant planet instability is likely to have occurred early in Solar System history. • The dynamical structure of Solar System can be explained by giant planet instability. • The early evolution of giant planets is used to get the timing of the instability. • The giant planet instability is likely to have occurred early in Solar System. [ABSTRACT FROM AUTHOR]
- Published
- 2020
- Full Text
- View/download PDF
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