Migration of giant planets in planetesimal discs

Popolo, A. Del; Gambera, M.; Ercan, E. N.

doi:10.1046/j.1365-8711.2001.04517.x

Cited by 13 publications

(28 citation statements)

References 68 publications

(130 reference statements)

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“…Some authors have also proposed scenarios in which migration and formation were concurrent (Terquem, Papaloizou & Nelson 2000). We refer the reader to Del Popolo et al (2001, hereafter DP1) and Del Popolo & Ekşi (2002, hereafter DP2) for a detailed discussion of the different mechanisms that have been proposed to explain the presence of planets at small orbital distances: (i) dynamical instabilities in a system of giant planets (Rasio & Ford 1996; Weidenshilling & Marzari 1996), (ii) ‘migration instability’ (Murray et al 1998), (iii) tidal interaction with a gaseous nebula (Goldreich & Tremaine 1979, 1980; Ward 1986; Lin, Bodenheimer & Richardson 1996; Ward 1997) and (iv) dynamical friction between the planet and a planetesimal disc (DP1).…”

Section: Introductionmentioning

confidence: 99%

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Evolution of planetesimal discs and planetary migration

Popolo

Yeşilyurt

Ercan

2003

Monthly Notices of the Royal Astronomical Society

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In this paper, we further develop the model for the migration of planets introduced by Del Popolo, Gambera & Ercan and extended to time‐dependent planetesimal accretion discs by Del Popolo & Ekşi. More precisely, the assumption of Del Popolo & Ekşi that the surface density in planetesimals is proportional to that of the gas was released. Indeed, the evolution of the radial distribution of solids is governed by many processes: gas–solid coupling, coagulation, sedimentation, evaporation/condensation, so that the distribution of planetesimals emerging from a turbulent disc does not necessarily reflect that of the gas. In order to describe this evolution we use a method developed by Stepinski & Valageas, which, using a series of simplifying assumptions, is able to simultaneously follow the evolution of gas and solid particles for up to 107 yr. This model is based on the premise that the transformation of solids from dust to planetesimals occurs through hierarchical coagulation. Then, the distribution of planetesimals obtained after 107 yr is used to study the migration rate of a giant planet through the migration model introduced by Del Popolo, Gambera & Ercan. This allows us to investigate the dependence of the migration rate on the disc mass, on its time evolution and on the value of the dimensionless viscosity parameter α. We find that in the case of discs having a total mass of 10−3–10−1 M⊙, and 10−4 < α < 10−1, planets can migrate inward over a large distance while if Md < 10−3, M⊙ the planets remain almost at their initial position for α > 10−3 and only in the case where α < 10−3 do the planets move to a minimum value of orbital radius of ≃2 au. Moreover, the observed distribution of planets in the period range 0–20 d can be easily obtained from our model. Therefore, dynamical friction between planets and the planetesimal disc provides a good mechanism to explain the properties of observed extrasolar giant planets.

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Section: Introductionmentioning

confidence: 99%

“…The main approximation used in this model is to associate one grain size to a given radius and time. Then, we use the radial distribution of planetesimals predicted by this model to estimate the planet migration, which is computed as in Del Popolo et al (2001).…”

Section: Introductionmentioning

confidence: 99%

Evolution of planetesimal discs and planetary migration

Popolo

Yeşilyurt

Ercan

2003

Monthly Notices of the Royal Astronomical Society

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“…Levison & Stewart (2001) argued that the ‘standard’ model for the formations of Uranus and Neptune was not correct, and they concluded that Jovian planets most probably experienced orbital expansions. In fact, some indirect evidence, including observations of extrasolar systems, has been found and diverse models have been proposed (Del Popolo, Gambera & Ercan 2001). Planets may migrate outward or inward, depending on the specific dynamical processes that they underwent.…”

Section: Introductionmentioning

confidence: 99%

Stochastic effects in the planet migration and orbital distribution of the Kuiper Belt

Li-yong

Sun

Zhou

et al. 2002

Monthly Notices of the Royal Astronomical Society

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Assuming the Jovian planets experienced smooth orbital migrations, Malhotra successfully explained some important features of the Kuiper Belt by the mechanism of resonance capture. However, the migration should really be stochastic. In this paper we numerically simulate numerous orbital evolutions of test particles under such stochastic planet migrations. The main results are as follows. Given the proper parameters, the concentration of objects in the 3 : 2 resonance is distinct, while very few objects enter the 2 : 1 resonance, and consequently, the orbital distribution of Kuiper Belt objects matches the observational data very well. The stochastic effects excite the orbital eccentricities and inclinations of objects in the non‐resonant regions. The introduction of stochastic effects also gives possible explanations of the mass depletion, and of the sources of the classical and scattered Kuiper Belt objects.

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“…Hot Jupiters are thought not to have formed in their short‐period orbits but to have migrated in from much larger radii early in the history of the Solar system (e.g. Nelson et al 2001; Del Popolo, Gambera & Ercan 2001). According to Burrows et al (2000), the ordinary contraction of the planet under gravity in the first few Myr after formation will be halted, but not reversed, by strong stellar insolation.…”

Section: Introductionmentioning

confidence: 99%

A search for the infrared spectroscopic signature of hot Jupiter planets

Lucas

Roche

2002

Monthly Notices of the Royal Astronomical Society

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We present the results of an attempt to detect the hottest ‘hot Jupiter’ planets directly in the thermal infrared. A simple method based upon high signal‐to‐noise ratio spectroscopy of the central star at low spectral resolution is described. In the 2–4 μm region the contrast ratio between planet and star is expected to be relatively low and the planetary spectrum should appear as a faint signal on top of the stellar spectrum, distinguished by edges of H2O absorption. No water edges were found to 3σ limits of one part in a few hundred in each case. These upper limits are compared with the irradiated planetary atmosphere models of Barman, Hauschildt & Allard to derive upper limits on the size of the hot Jupiters, which are expected to be somewhat larger than Jupiter. If reasonably strong H2O absorption occurs in these objects then typical upper limits of R < 3 RJup are derived, the precision being limited by the stability of telluric transmission. Only a modest improvement in precision is needed (e.g. with space‐based instruments) to reach the range of greatest interest (1 < R < 2 RJup).

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Migration of giant planets in planetesimal discs

Cited by 13 publications

References 68 publications

Evolution of planetesimal discs and planetary migration

Evolution of planetesimal discs and planetary migration

Stochastic effects in the planet migration and orbital distribution of the Kuiper Belt

A search for the infrared spectroscopic signature of hot Jupiter planets

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