Eccentric Extrasolar Planets: The Jumping Jupiter Model

Marzari, F.

doi:10.1006/icar.2001.6786

Cited by 277 publications

(297 citation statements)

References 27 publications

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“…As discussed previously, the large eccentricities (and obliquities) of the extrasolar planet population suggest that planet-planet gravitational scattering ("Jumping Jupiters") may be important (e.g. [7,29,55]), and this is likely to occur toward the end of the gas disk lifetime when its ability to damp orbital eccentricities is diminished. When combined with tidal interaction with the central star, planet-planet scattering onto highly eccentric orbits can form short-period planets that have not migrated toward the central star while accreting from the circumstellar disk.…”

Section: Scenariomentioning

confidence: 84%

“…the Jumping Jupiter mechanism, [7,29,55]) can supply an alternate evolutionary path to the previously described picture derived from the Solar System. The dynamical effects of the migrating planet on the protoplanetary disk would replace the slow erosion due to the interplay between planetary embryos and orbital resonances with the giant planets, but the end result would be analogous: the reshuffling of material from different regions of the protoplanetary disk and the depletion of the population of planetesimals with a consequence capture of part of the removed population by the giant planets.…”

Section: Post-formation Evolution Late Accretion and Protoplanetary mentioning

confidence: 91%

“…This can arise through the exchange of angular momentum with the circumstellar disk in which the forming planets are embedded (see e.g. [5,38], and references therein), and through the so-called "Jumping Jupiters" mechanism [7,29,55], which invokes multiple planetary encounters with a chaotic exchange of angular momentum and energy between the bodies involved. Each of these migration mechanisms has different implications for the chemical make-up of the planetary atmosphere, as migration through a disk allows the planet to accrete from regions with varying chemical abundances.…”

Section: Introductionmentioning

confidence: 99%

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The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

2014

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Over the last twenty years, the search for extrasolar planets has revealed the rich diversity of outcomes from the formation and evolution of planetary systems. In order to fully understand how these extrasolar planets came to be, however, the orbital and physical data we possess are not enough, and they need to be complemented with information about the composition of the exoplanets. Ground-based and space-based observations provided the first data on the atmospheric composition of a few extrasolar planets, but a larger and more detailed sample is required before we can fully take advantage of it. The primary goal of a dedicated space mission like the Exoplanet Characterization Observatory (EChO) proposal is to fill this gap and to expand the limited data we possess by performing a systematic survey of extrasolar planets. The full exploitation of the data that space-based and ground-based facilities will provide in the near future, however, requires knowledge about the sources and sinks of the chemical species and molecules that will be observed. Luckily, the study of the past history of the Solar System provides several indications about the effects of processes like migration, late accretion and secular impacts, and on the time they occur in the life of planetary systems. In this work we will review what is

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Section: Scenariomentioning

confidence: 84%

Section: Post-formation Evolution Late Accretion and Protoplanetary mentioning

confidence: 91%

Section: Introductionmentioning

confidence: 99%

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The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

2014

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“…Many of these have shown that the most common outcome of gravitational scattering by close encounters is the hyperbolic ejection of one planet, the 'survivors' having significant values of eccentricity and mutual inclination (e.g. Marzari & Weidenschilling 2002, Chatterjee et al 2008, Jurić & Tremaine 2008. These works focused on gas-free systems, assuming that systems that are relatively compact when the gas nebula dissipates will undergo planet-planet scattering after a relatively short time.…”

Section: Introductionmentioning

confidence: 99%

Trapping in three-planet resonances during gas-driven migration

Libert

Tsiganis

2011

Celest Mech Dyn Astr

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We study the establishment of three-planet resonances -similar to the Laplace resonance in the Galilean satellites -and their effects on the mutual inclinations of the orbital planes of the planets, assuming that the latter undergo migration in a gaseous disc. In particular, we examine the resonance relations that occur, by varying the physical and initial orbital parameters of the planets (mass, initial semi-major axis and eccentricity) as well as the parameters of the migration forces (migration rate and eccentricity damping rate), which are modeled here through a simplified analytic prescription. We find that, in general, for planetary masses below 1.5 M J , multiple-planet resonances of the form n 3 :n 2 :n 1 =1:2:4 and 1:3:6 are established, as the inner planets, m 1 and m 2 , get trapped in a 1:2 resonance and the outer planet m 3 subsequently is captured in a 1:2 or 1:3 resonance with m 2 . For mild eccentricity damping, the resonance pumps the eccentricities of all planets on a relatively short time-scale, to the point where they enter an inclination-type resonance (as in Libert & Tsiganis 2011); then mutual inclinations can grow to ∼ 35 • , thus forming a "3-D system". On the other hand, we find that trapping of m 2 in a 2:3 resonance with m 1 occurs very rarely, for the range of masses used here, so only two cases of capture in a respective three-planet resonance were found. Our results suggest that trapping in a three-planet resonance can be common in exoplanetary systems, provided that the planets are not very massive. Inclination pumping could then occur relatively fast, provided that eccentricity damping is not very efficient so that at least one of the inner planets acquires an orbital eccentricity higher than e = 0.3.

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“…Another important result derived from these observations is the possibility to determine whether short orbital period transiting planets move in the same direction of the stellar spin, indicating the existence of strong dynamical interactions between the parent star and its planet. Measurements of the Rossiter-McLaughlin effect thus provide relevant residual evidence of planet formation and migration processes, as well as dynamical interactions with perturbing bodies (Marzari & Weidenschilling 2002).…”

Section: Introductionmentioning

confidence: 99%

Characterization of the HD 17156 planetary system

Barbieri¹,

Alonso²,

Desidera

et al. 2009

A&A

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Aims. We present data to improve the known parameters of the HD 17156 system (peculiar due to the eccentricity and long orbital period of its transiting planet) and constrain the presence of stellar companions. Methods. Photometric data were acquired for 4 transits, and high precision radial velocity measurements were simultaneously acquired with the SARG spectrograph at TNG for one transit. The template spectra of HD 17156 was used to derive effective temperature, gravity, and metallicity. A fit of the photometric and spectroscopic data was performed to measure the stellar and planetary radii, and the spin-orbit alignment. Planet orbital elements and ephemeris were derived from the fit. Near infrared adaptive optic images were acquired with the AdOpt module of TNG. Results. We found that the star has a radius of R S = 1.44 ± 0.03 R and the planet R P = 1.02 ± 0.08 R J . The transit ephemeris is T c = 2 454 756.73134 ± 0.00020 + N · 21.21663 ± 0.00045 BJD. Analysis of the Rossiter-Mclaughlin effect shows that the system is spin orbit aligned with an angle β = 4.8 • ± 5.3 • . The analysis of high resolution images did not reveal any stellar companion with a projected separation between of 150 and 1 000 AU from HD 17156.

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Eccentric Extrasolar Planets: The Jumping Jupiter Model

Cited by 277 publications

References 27 publications

The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

Trapping in three-planet resonances during gas-driven migration

Characterization of the HD 17156 planetary system

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