A STATISTICAL RECONSTRUCTION OF THE PLANET POPULATION AROUND<i>KEPLER</i>SOLAR-TYPE STARS

Silburt, Ari; Gaidos, Eric; Wu, Yanqin

doi:10.1088/0004-637x/799/2/180

Cited by 159 publications

(131 citation statements)

References 65 publications

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“…Recent studies (Youdin 2011;Fressin et al 2013;Petigura et al 2013;Weiss & Marcy 2014;Marcy et al 2014;Silburt et al 2015;Rogers 2015) have shown that the size distribution of extrasolar planets peaks at about ∼2 Earth radii (between 1.5 and <3.0). This same pattern is clearly present in the current planet candidate population (Burke et al 2014).…”

Section: Discussionmentioning

confidence: 99%

Accretion of Uranus and Neptune from inward-migrating planetary embryos blocked by Jupiter and Saturn

Izidoro

Morbidelli

Raymond

et al. 2015

A&A

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Reproducing Uranus and Neptune remains a challenge for simulations of solar system formation. The ice giants' peculiar obliquities suggest that they both suffered giant collisions during their formation. Thus, there must have been an epoch of accretion dominated by collisions among large planetary embryos in the primordial outer solar system. We test this idea using N-body numerical simulations including the effects of a gaseous protoplanetary disk. One strong constraint is that the masses of the ice giants are very similarthe Neptune and Uranus mass ratio is ∼1.18. We show that similar-sized ice giants do indeed form by collisions between planetary embryos beyond Saturn. The fraction of successful simulations varies depending on the initial number of planetary embryos in the system, their individual and total masses. Similar-sized ice giants are consistently reproduced in simulations starting with five to ten planetary embryos with initial masses of ∼3-6 M ⊕ . We conclude that accretion from a population of planetary embryos is a plausible scenario for the origin of Uranus and Neptune.

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Section: Discussionmentioning

confidence: 99%

Accretion of Uranus and Neptune from inward-migrating planetary embryos blocked by Jupiter and Saturn

Izidoro

Morbidelli

Raymond

et al. 2015

A&A

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“…All red (r − J > 2.2) stars were classified as dwarf or giant stars based on available spectra and photometry. The intrinsic, de-biased planet population with orbital period P < 180 d was constructed using the method of iterative Monte Carlo (Cappe et al 2007), where a synthetic input population of planets is evolved by repeated passage through a detection simulation (Silburt et al 2015). Host stars and planets are randomized with the assumption that, within the sample, their properties are uncorrelated.…”

Section: Methodsmentioning

confidence: 99%

A minimum mass nebula for M dwarfs

Gaidos

2017

Monthly Notices of the Royal Astronomical Society: Letters

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Recently revealed differences in planets around M dwarf vs. solar-type stars could arise from differences in their primordial disks, and surveys of T Tauri stars find a correlation between stellar mass and disk mass. "Minimum" disks have been reconstructed for the Solar System and solar-type stars and here this exercise is performed for M dwarfs using Kepler-detected planets. Distribution of planet mass between current orbits produces a disk with total mass of ≈0.009M ⊙ and a power-law profile with index α = 2.2. Disk reconstruction from the output of a forward model of planet formation indicates that the effect of detection bias on disk profile is slight and that the observed scatter in planet masses and semi-major axes is consistent with a universal disk profile. This nominal M dwarf disk is more centrally concentrated than those inferred around the solar-type stars observed by Kepler, and the mass surface density beyond 0.02 AU is sufficient for in situ accretion of planets as single embryos. The mass of refractory solids within 0.5 AU is 5.6M ⊕ compared to 4M ⊕ for solar-type stars, in contrast with the trend with total disk mass. The total solids beyond 0.5 AU is sufficient for the core of at least one giant planet.

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“…In contrast to the small fraction of stars with warm debris disks, rocky planets within 1 AU appear to be fairly common companions to solar-type stars (Youdin 2011b;Fang & Margot 2012;Batalha et al 2013;Foreman-Mackey et al 2014;Silburt et al 2015;Winn & Fabrycky 2015). Although the false positive rate is uncertain, recent attempts to confirm Kepler candidates with ground-based and other space-based observations suggest false positive rates ranging from ∼ 10% to 75% for various ranges of planet masses (e.g., Morton & Johnson 2011;Santerne et al 2012;Fressin et al 2013;Sliski & Kipping 2014;Désert et al 2015;Colón et al 2015;Santerne et al 2016;Coughlin et al 2016;Mullally et al 2016;Morton et al 2016).…”

Section: Earth Mass Planets At 025-1 Au Are Fairly Commonmentioning

confidence: 99%

Rocky Planet Formation: Quick and Neat

Kenyon

Najita

Bromley

2016

ApJ

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We reconsider the commonly held assumption that warm debris disks are tracers of terrestrial planet formation. The high occurrence rate inferred for Earthmass planets around mature solar-type stars based on exoplanet surveys (∼ 20%) stands in stark contrast to the low incidence rate (≤ 2%-3%) of warm dusty debris around solar-type stars during the expected epoch of terrestrial planet assembly (∼ 10 Myr). If Earth-mass planets at AU distances are a common outcome of the planet formation process, this discrepancy suggests that rocky planet formation occurs more quickly and/or is much neater than traditionally believed, leaving behind little in the way of a dust signature. Alternatively, the incidence rate of terrestrial planets has been overestimated or some previously unrecognized physical mechanism removes warm dust efficiently from the terrestrial planet region. A promising removal mechanism is gas drag in a residual gaseous disk with a surface density 10 −5 of the minimum mass solar nebula.

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A STATISTICAL RECONSTRUCTION OF THE PLANET POPULATION AROUNDKEPLERSOLAR-TYPE STARS

Cited by 159 publications

References 65 publications

Accretion of Uranus and Neptune from inward-migrating planetary embryos blocked by Jupiter and Saturn

Accretion of Uranus and Neptune from inward-migrating planetary embryos blocked by Jupiter and Saturn

A minimum mass nebula for M dwarfs

Rocky Planet Formation: Quick and Neat

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