Challenges in planet formation

Morbidelli, Alessandro; Raymond, Sean N.

doi:10.1002/2016je005088

Cited by 168 publications

(136 citation statements)

References 204 publications

(294 reference statements)

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“…Thus, our results are in good agreement with the timing and sequence of events predicted in the core accretion model for the formation of Jupiter (1). One important implication of this result is that, because Jupiter acted as a barrier against inward transport of solids across the disk, the inner Solar System remained relatively mass deficient, possibly explaining its lack of any "super-Earths" (34,35).…”

Section: Growth History Of Jupitersupporting

confidence: 86%

Age of Jupiter inferred from the distinct genetics and formation times of meteorites

Kruijer

Burkhardt

Budde

et al. 2017

Proc. Natl. Acad. Sci. U.S.A.

515

586

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Significance Jupiter is the most massive planet of the Solar System and its presence had an immense effect on the dynamics of the solar accretion disk. Knowing the age of Jupiter, therefore, is key for understanding how the Solar System evolved toward its present-day architecture. However, although models predict that Jupiter formed relatively early, until now, its formation has never been dated. Here we show through isotope analyses of meteorites that Jupiter’s solid core formed within only ∼1 My after the start of Solar System history, making it the oldest planet. Through its rapid formation, Jupiter acted as an effective barrier against inward transport of material across the disk, potentially explaining why our Solar System lacks any super-Earths.

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Section: Growth History Of Jupitersupporting

confidence: 86%

Age of Jupiter inferred from the distinct genetics and formation times of meteorites

Kruijer

Burkhardt

Budde

et al. 2017

Proc. Natl. Acad. Sci. U.S.A.

515

586

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“…These zero torque locations move radially inwards as the disc evolves over time (Lyra et al 2010). It can be seen from Bitsch et al (2015) and Morbidelli & Raymond (2016) that at late times in the evolution of a disc the zero torque boundary follows a curve where essentially the planet mass falls off with radial location, as seen in our observational results, though the slope of this boundary is yet to be analysed in detail and the simulations are limited to outer regions of the disc. Further study of other planet-disk processes including gap-opening and migration is needed to fully assess the importance of the disc phase.…”

Section: Zero-torque Locationsupporting

confidence: 69%

A Gap in the Mass Distribution for Warm Neptune and Terrestrial Planets

Meru

Kennedy

Veras

2019

ApJL

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Structure in the planet distribution provides an insight into the processes that shape the formation and evolution of planets. The Kepler mission has led to an abundance of statistical discoveries in regards to planetary radius, but the number of observed planets with measured masses is much smaller. By incorporating results from recent mass determination programs, we have discovered a new gap emerging in the planet population for sub-Neptune mass planets with orbital periods less than 20 days. The gap follows a slope of decreasing mass with increasing orbital period, has a width of a few M ⊕ , and is potentially completely devoid of planets. Fitting gaussian mixture models to the planet population in this region favours a bimodel distribution over a unimodel one with a reduction in Bayesian Information Criterion (BIC) of 19.9, highlighting the gap significance. We discuss several processes which could generate such a feature in the planet distribution, including a pileup of planets above the gap region, tidal interactions with the host star, dynamical interactions with the disk, with other planets, or with accreting material during the formation process.

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“…In this case, the lack of a substantial inner disk eliminates some of the proposed mechanisms involving accretion (Bouvier et al 2013) or vertical structures in a disk (Ansdell et al 2016b). Impact disruption of asteroidal bodies or giant impacts during the final phase of rocky planet formation (Morbidelli & Raymond 2016) have been invoked to explain warm dust around 30-50 Myr-old RZ Piscium, the 25 Myrold β Pictoris Moving Group member HD 172555 (Johnson et al 2012), and ID8, a star with a rapidly time-varying excess in the ∼35 Myr cluster NGC 2547 (Su et al 2019). Something analogous to these impact-driven disks might explain the excess infrared emission of 125 Myr-old HD 240779.…”

Section: Summary and Discussionmentioning

confidence: 99%

Planetesimals around stars with TESS (PAST) – I. Transient dimming of a binary solar analogue at the end of the planet accretion era

Gaidos

Jacobs

LaCourse³

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report detection of quasi-periodic (1.5-day) dimming of HD 240779, the solar-mass primary in a 5" visual binary (also TIC 284730577), by the Transiting Exoplanet Survey Satellite. This dimming, as has been shown for other "dipper" stars, is likely due to occultation by circumstellar dust. The barycentric space motion, lithium abundance, rotation, and chromospheric emission of the stars in this system point to an age of ≈125 Myr, and possible membership in the AB Doradus moving group. As such it occupies an important but poorly explored intermediate regime of stars with transient dimming between young stellar objects in star forming regions and main sequence stars, and between UX Orionis-type Ae/Be stars and M-type "dippers". HD 240779, but not its companion BD+10 714B, has WISE -detected excess infrared emission at 12 and 22 µm indicative of circumstellar dust. We propose that infrared emission is produced by collisions of planetesimals during clearing of a residual disk at the end of rocky planet formation, and that quasi-periodic dimming is produced by the rapid disintegration of a 100 km planetesimal near the silicate evaporation radius. Further studies of this and similar systems will illuminate a poorly understood final phase of rocky planet formation like that which produced the inner Solar System.

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Challenges in planet formation

Cited by 168 publications

References 204 publications

Age of Jupiter inferred from the distinct genetics and formation times of meteorites

Age of Jupiter inferred from the distinct genetics and formation times of meteorites

A Gap in the Mass Distribution for Warm Neptune and Terrestrial Planets

Planetesimals around stars with TESS (PAST) – I. Transient dimming of a binary solar analogue at the end of the planet accretion era

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