Orbital migration and the frequency of giant planet formation

Trilling, David E.; Lunine, Jonathan I.; Benz, W.

doi:10.1051/0004-6361:20021108

Cited by 106 publications

(139 citation statements)

References 81 publications

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“…This close to the star, the disk structure is more complex than further out, due for example to magnetic field effects (Lin et al 1996) or tidal interactions (Trilling et al 2002), which influence the formation of planets entering this zone, by altering the accretion or the migration rate (Papaloizou & Terquem 1999). Also after formation, very close-in planets can be subject to mass loss by evaporation (Vidal-Madjar et al 2003;Baraffe 2004).…”

Section: Planets Very Close To the Starmentioning

confidence: 99%

Extrasolar planet population synthesis

Mordasini¹,

Alibert

Benz³

2009

A&A

Self Cite

527

551

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Context. With the high number of extrasolar planets discovered by now, it has become possible to use the properties of this planetary population to constrain theoretical formation models in a statistical sense. This paper is the first in a series in which we carry out a large number of planet population synthesis calculations within the framework of the core accretion scenario. We begin the series with a paper mainly dedicated to the presentation of our approach, but also the discussion of a representative synthetic planetary population of solar like stars. In the second paper we statistically compare the subset of detectable planets to the actual extrasolar planets. In subsequent papers, we shall extend the range of stellar masses and the properties of protoplanetary disks. Aims. The last decade has seen a large observational progress in characterizing both protoplanetary disks, and extrasolar planets. Concurrently, progress was made in developing complex theoretical formation models. The combination of these three developments allows a new kind of study: the synthesis of a population of planets from a model, which is compared with the actual population. Our aim is to obtain a general overview of the population, to check if we quantitatively reproduce the most important observed properties and correlations, and to make predictions about the planets that are not yet observable. Methods. Based as tightly as possible on observational data, we have derived probability distributions for the most important initial conditions for the planetary formation process. We then draw sets of initial conditions from these distributions and obtain the corresponding synthetic planets with our formation model. By repeating this step many times, we synthesize the populations. Results. Although the main purpose of this paper is the description of our methods, we present some key results: we find that the variation of the initial conditions in the limits occurring in nature leads to the formation of planets of wide diversity. This formation process is best visualized in planetary formation tracks in the mass-semimajor axis diagram, where different phases of concurrent growth and migration can be identified. These phases lead to the emergence of sub-populations of planets distinguishable in a mass-semimajor axis diagram. The most important ones are the "failed cores", a vast group of core-dominated low mass planets, the "horizontal branch", a sub-population of Neptune mass planets extending out to 6 AU, and the "main clump", a concentration of giant gaseous planets at around 0.3−2 AU.

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Section: Planets Very Close To the Starmentioning

confidence: 99%

Extrasolar planet population synthesis

Mordasini¹,

Alibert

Benz³

2009

A&A

Self Cite

527

551

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“…Trilling et al 1998;Nelson et al 2000). It also takes more time to open a gap in the disk for massive planets -eventually longer than the lifetime of the disk -and initiate type II migration (Trilling et al 2002).…”

Section: Low Migration Rate For Massive Planetsmentioning

confidence: 99%

Statistical properties of exoplanets

Udry

Mayor

Santos

2003

A&A

190

179

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Abstract.Interesting emerging observational properties of the period-mass distribution of extra-solar planets are discussed. New recent detections confirm the already emphasized lack of massive planets (m 2 sin i ≥ 2 M Jup ) on short-period orbits (P ≤ 100 days). Furthermore, we point out i) a shortage of planets in the 10-100 day period range as well as ii) a lack of light planets (m 2 sin i ≤ 0.75 M Jup ) on orbits with periods larger than ∼100 days. The latter feature is shown not to be due to smallnumber statistics with Monte-Carlo simulations. These observational period-related characteristics are discussed in the context of the migration process of exoplanets. They are found to be in agreement with recent simulations of planet interactions with viscous disks. The observed valley at a few tens of days in the period distribution is interpreted as a transition region between two categories of planets that suffered different migration scenarios. The lack of light planets on longer-period orbits and the corresponding intriguing sharp limit in mass is tentatively explained by the runaway migration process recently studied by Masset & Papaloizou (2003). The observed properties also have implications for the observation strategies of the on-going surveys and of future higher-precision searches.

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“…They encountered difficulties forming the planets within the required timescales of estimated disk lifetimes unless certain nebular parameters were set to unlikely values, but cautioned that there are still major uncertainties associated with the nebula model. Thus, it seems more likely that gas planets form at large distances (e 5 AU) and migrate toward their observed positions, a process possibly caused by disk-planet interactions (see, e.g., Papaloizou & Terquem 1999;Trilling, Lunine, & Benz 2002, and references therein). On the other hand, Ikoma, Emori, & Nakazawa (2001) do not exclude the possibility of in situ formation of extrasolar giant planets.…”

Section: Stellar Metallicity and Giant Planet Formationmentioning

confidence: 99%

Abundance Analysis of Planetary Host Stars. I. Differential Iron Abundances

Heiter¹,

Luck²

2003

101

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We present atmospheric parameters and iron abundances derived from high-resolution spectra for three samples of dwarf stars: stars that are known to host close-in giant planets (CGP), stars for which radial velocity data exclude the presence of a close-in giant planetary companion (no-CGP), as well as a random sample of dwarfs with a spectral type and magnitude distribution similar to that of the planetary host stars (control). All stars have been observed with the same instrument and have been analyzed using the same model atmospheres, atomic data, and equivalent width modeling program. Abundances have been derived differentially to the Sun, using a solar spectrum obtained with Callisto as the reflector with the same instrumentation. We find that the iron abundances of CGP dwarfs are on average 0.22 dex greater than that of no-CGP dwarfs. The iron abundance distributions of both the CGP and no-CGP dwarfs are different than that of the control dwarfs, while the combined iron abundances have a distribution that is very similar to that of the control dwarfs. All four samples (CGP, no-CGP, combined, and control) have different effective temperature distributions. We show that metal enrichment occurs only for CGP dwarfs with temperatures just below solar and %300 K higher than solar, whereas the abundance difference is insignificant at T eff around 6000 K.

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Orbital migration and the frequency of giant planet formation

Cited by 106 publications

References 81 publications

Extrasolar planet population synthesis

Extrasolar planet population synthesis

Statistical properties of exoplanets

Abundance Analysis of Planetary Host Stars. I. Differential Iron Abundances

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