The known extrasolar multiple-planet systems share a surprising dynamical attribute: they cluster just beyond the Hill stability boundary. Here we show that the planet-planet scattering model, which ...naturally explains the observed exoplanet eccentricity distribution, can reproduce the observed distribution of dynamical configurations. We calculated how each of our scattered systems would appear over an appropriate range of viewing geometries; as Hill stability is weakly dependent on the masses, the mass-inclination degeneracy does not significantly affect our results. We consider a wide range of initial planetary mass distributions and find that some are poor fits to the observed systems. In fact, many of our scattering experiments overproduce systems very close to the stability boundary. The distribution of dynamical configurations of two-planet systems actually may provide better discrimination between scattering models than the distribution of eccentricity. Our results imply that, at least in their inner regions which are weakly affected by gas or planetesimal disks, planetary systems should be "packed", with no large gaps between planets.
Direct imaging searches have begun to detect planetary and brown dwarf companions and to place constraints on the presence of giant planets at large separations from their host star. This work helps ...to motivate such planet searches by predicting a population of young giant planets that could be detectable by direct imaging campaigns. Both the classical core accretion and the gravitational instability model for planet formation are hard-pressed to form long-period planets in situ. Here, we show that dynamical instabilities among planetary systems that originally formed multiple giant planets much closer to the host star could produce a population of giant planets at large (~100 AU - 100000 AU) separations. We estimate the limits within which these planets may survive, quantify the efficiency of gravitational scattering into both stable and unstable wide orbits, and demonstrate that population analyses must take into account the age of the system. We predict that planet scattering creates a population of detectable giant planets on wide orbits that decreases in number on timescales of ~10 Myr. We demonstrate that several members of such populations should be detectable with current technology, quantify the prospects for future instruments, and suggest how they could place interesting constraints on planet formation models.
The significant orbital eccentricities of most giant extrasolar planets may have their origin in the gravitational dynamics of initially unstable multiple planet systems. In this work, we explore the ...dynamics of two close planets on inclined orbits through both analytical techniques and extensive numerical scattering experiments. We derive a criterion for two equal mass planets on circular inclined orbits to achieve Hill stability, and conclude that significant radial migration and eccentricity pumping of both planets occurs predominantly by 2:1 and 5:3 mean motion resonant interactions. Using Laplace-Lagrange secular theory, we obtain analytical secular solutions for the orbital inclinations and longitudes of ascending nodes, and use those solutions to distinguish between the secular and resonant dynamics which arise in numerical simulations. We also illustrate how encounter maps, typically used to trace the motion of massless particles, may be modified to reproduce the gross instability seen by the numerical integrations. Such a correlation suggests promising future use of such maps to model the dynamics of more coplanar massive planet systems.
The recent discoveries of massive planets on ultra-wide orbits of HR 8799 (Marois et al. 2008) and Fomalhaut (Kalas et al. 2008) present a new challenge for planet formation theorists. Our goal is to ...figure out which of three giant planet formation mechanisms--core accretion (with or without migration), scattering from the inner disk, or gravitational instability--could be responsible for Fomalhaut b, HR 8799 b, c and d, and similar planets discovered in the future. This paper presents the results of numerical experiments comparing the long-period planet formation efficiency of each possible mechanism in model A star, G star and M star disks. First, a simple core accretion simulation shows that planet cores forming beyond 35 AU cannot reach critical mass, even under the most favorable conditions one can construct. Second, a set of N-body simulations demonstrates that planet-planet scattering does not create stable, wide-orbit systems such as HR 8799. Finally, a linear stability analysis verifies previous work showing that global spiral instabilities naturally arise in high-mass disks. We conclude that massive gas giants on stable orbits with semimajor axes greater than 35 AU form by gravitational instability in the disk. We recommend that observers examine the planet detection rate as a function of stellar age, controlling for planet dimming with time. If planet detection rate is found to be independent of stellar age, it would confirm our prediction that gravitational instability is the dominant mode of producing detectable planets on wide orbits. We also predict that the occurrence ratio of long-period to short-period gas giants should be highest for M dwarfs due to the inefficiency of core accretion and the expected small fragment mass in their disks.
Observations of structure in circumstellar debris discs provide circumstantial evidence for the presence of massive planets at large (several tens of au) orbital radii, where the timescale for planet ...formation via core accretion is prohibitively long. Here, we investigate whether a population of distant planets can be produced via outward migration subsequent to formation in the inner disc. Two possibilities for significant outward migration are identified. First, cores that form early at radii of around 10 au can be carried to larger radii via gravitational interaction with the gaseous disc. This process is efficient if there is strong mass loss from the disc - either within a cluster or due to photoevaporation from a star more massive than the Sun - but does not require the extremely destructive environment found, for example, in the core of the Orion Nebula. We find that, depending upon the disc model, gas disc migration can yield massive planets (several Jupiter masses) at radii of around 20-50 au. Second, interactions within multiple planet systems can drive the outer planet into a large, normally highly eccentric orbit. A series of scattering experiments suggests that this process is most efficient for lower mass planets within systems of unequal mass ratio. This mechanism is a good candidate for explaining the origin of relatively low mass giant planets in eccentric orbits at large radii.
We present new precision radial velocities and a three-planet Keplerian orbit fit for the V = 8.5, G5 V star HIP 14810. We began observing this star at Keck Observatory as part of the N2K Planet ...Search Project. Wright et al. (2007) announced the inner two planets to this system, and subsequent observations have revealed the outer planet planet and the proper orbital solution for the middle planet. The planets have minimum masses of 3.9, 1.3, and 0.6 M_Jup and orbital periods of 6.67, 147.7, and 952 d, respectively. We have numerically integrated the family of orbital solutions consistent with the data and find that they are stable for at least 10^6 yr. Our photometric search shows that the inner planet does not transit.
We present new radial velocities from Keck Observatory and both Newtonian and Keplerian solutions for the triple-planet system orbiting HD 37124. The orbital solution for this system has improved ...dramatically since the third planet was first reported in Vogt et al. 2005 with an ambiguous orbital period. We have resolved this ambiguity, and the outer two planets have an apparent period commensurability of 2:1. A dynamical analysis finds both resonant and non-resonant configurations consistent with the radial velocity data, and constrains the mutual inclinations of the planets to be less than about 30 degrees. We discuss HD 37124 in the context of the other 19 exoplanetary systems with apparent period commenserabilities, which we summarize in a table. We show that roughly one in three well-characterized multiplanet systems has a apparent low-order period commensuribility, which is more than would naively be expected if the periods of exoplanets in known multiplanet systems were drawn randomly from the observed distribution of planetary orbital periods.
Le partage des savoirs se décline sous différentes facettes dans ce numéro. Qu’il s’agisse de la prise en charge pluridisciplinaire des RPS ou du transfert aux novices des savoirs professionnels, le ...partage des savoirs est au cœur des pratiques professionnelles. On le retrouve également au centre du travail d’articulation des cadres de proximité dans l’horticulture. Le partage des savoirs entre disciplines permet aussi d’élargir la compréhension du rapport subjectif au travail dans le domaine de la construction au Brésil. Enfin, la fermeture au partage des savoirs peut entraîner de nombreux freins à la reconnaissance par les employeurs de leur responsabilité face aux maladies professionnelles, comme dans le cas des cancers professionnels en France.
O objetivo deste estudo foi comparar a atividade eletromiográfica (EMG) dos músculos reto femoral, bíceps femoral, tibial anterior e sóleo no agachamento, associando a posição de tronco ereto com 2 ...ângulos de flexão do joelho (40° e 60°) e a posição de tronco fletido a 45° com 3 ângulos de flexão do joelho (40°, 60° e 90°). Todas as combinações foram realizadas com e sem acréscimo de carga (10kg). A amostra foi composta por 12 indivíduos saudáveis com idade de 21,1 ± 2,5 anos e massa corporal de 62,8 ± 7,4kg. O EMG dos músculos citados foi registrado, isometricamente, em 10 posições de agachamento. Para a análise estatística foi aplicada ANOVA Two-Way de Friedman e o teste Post-Hoc de Newman-Keuls. Os resultados mostraram co-ativação entre os músculos reto femoral e bíceps femoral nas posições de tronco fletido e joelho em flexão de 40º e, entre os músculos reto femoral e sóleo, nas demais posições (p < 0,05). Houve co-ativação entre o tibial anterior e bíceps femoral com o joelho a 40º, com o tronco ereto e fletido e, entre o tibial anterior e sóleo, nas demais posições (p < 0,05). Quanto à ativação muscular isolada, a maior flexão do joelho no agachamento foi um fator determinante para maior ativação dos músculos, exceto para o sóleo. A posição do tronco e a carga adicional de 10kg influenciaram a ativação muscular do reto femoral, a 60° de flexão de joelho, na qual o tronco ereto proporcionou maior ativação. E para o bíceps femoral, a 40° de flexão de joelho, na qual o tronco flexionado proporcionou maior ativação. A co-ativação entre o reto femoral e o bíceps femoral na posição de tronco fletido, e entre o reto femoral e o sóleo nas demais posições, apontam para novas possibilidades de exercícios na reabilitação.
The aim of this study was to compare the electromyographic (EMG) activity of the femoris rectus, femoris biceps, tibialis anterior and soleus muscles in squatting, associating the trunk in erect position with two angles of knee flexion (40° and 60°) and the trunk at 45° flexion with three angles of knee flexion (40°, 60° and 90°). All associations were performed with and without additional load (10 kg). The sample was composed of 12 healthy individuals with mean age of 21.1 ± 2.5 years and weight of 62.8 ± 7.4 kg. The EMG of the cited muscles was isometrically registered in 10 squatting positions. For statistical analysis, Friedman Two-Way ANOVA and the Newman-Keuls Post-Hoc test were used. The results showed co-activation between the femoris rectus and femoris biceps muscles with the trunk in flexion and at 40° of knee flexion and between the femoris rectus and soleus muscles in the other positions considered (p < 0.05). It was also possible to observe co-activation between tibialis anterior and femoris biceps muscles with knee at 40° and 60° of flexion, with the trunk erect and in flexion and between the tibialis anterior and soleus muscles in the other positions (p < 0.05). Concerning isolated muscular activation, higher knee flexion in squatting was an important factor to greater muscles activation, except for the soleus. Trunk position and the additional load of 10 kg have influenced in the muscular activation of the femoris rectus at 60° of knee flexion, in which the erect trunk provided more activation. The femoris biceps presented greater activation when the knee was in 40° of flexion and the trunk flexioned. The co-activation between the femoris rectus and biceps with the trunk in flexion, and between the femoris rectus and soleus in the other positions, lead to new possibilities of exercises in rehabilitation.
O objetivo deste estudo foi comparar a atividade eletromiográfica (EMG) dos músculos reto femoral, bíceps femoral, tibial anterior e sóleo no agachamento, associando a posição de tronco ereto com 2 ...ângulos de flexão do joelho (40° e 60°) e a posição de tronco fletido a 45° com 3 ângulos de flexão do joelho (40°, 60° e 90°). Todas as combinações foram realizadas com e sem acréscimo de carga (10kg). A amostra foi composta por 12 indivíduos saudáveis com idade de 21,1 ± 2,5 anos e massa corporal de 62,8 ± 7,4kg. O EMG dos músculos citados foi registrado, isometricamente, em 10 posições de agachamento. Para a análise estatística foi aplicada ANOVA Two-Way de Friedman e o teste Post-Hoc de Newman-Keuls. Os resultados mostraram co-ativação entre os músculos reto femoral e bíceps femoral nas posições de tronco fletido e joelho em flexão de 40º e, entre os músculos reto femoral e sóleo, nas demais posições (p < 0,05). Houve co-ativação entre o tibial anterior e bíceps femoral com o joelho a 40º, com o tronco ereto e fletido e, entre o tibial anterior e sóleo, nas demais posições (p < 0,05). Quanto à ativação muscular isolada, a maior flexão do joelho no agachamento foi um fator determinante para maior ativação dos músculos, exceto para o sóleo. A posição do tronco e a carga adicional de 10kg influenciaram a ativação muscular do reto femoral, a 60° de flexão de joelho, na qual o tronco ereto proporcionou maior ativação. E para o bíceps femoral, a 40° de flexão de joelho, na qual o tronco flexionado proporcionou maior ativação. A co-ativação entre o reto femoral e o bíceps femoral na posição de tronco fletido, e entre o reto femoral e o sóleo nas demais posições, apontam para novas possibilidades de exercícios na reabilitação.
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