Planet formation and migration near the silicate sublimation front in protoplanetary disks

@article{Flock2019PlanetFA,
  title={Planet formation and migration near the silicate sublimation front in protoplanetary disks},
  author={Mario Flock and Neal J. Turner and Gijs D. Mulders and Yasuhiro Hasegawa and R. P. Nelson and Bertram Bitsch},
  journal={Astronomy \& Astrophysics},
  year={2019}
}
Context. The increasing number of newly detected exoplanets at short orbital periods raises questions about their formation and migration histories. Planet formation and migration depend heavily on the structure and dynamics of protoplanetary disks. A particular puzzle that requires explanation arises from one of the key results of the Kepler mission, namely the increase in the planetary occurrence rate with orbital period up to 10 days for F, G, K and M stars. Aims. We investigate the… 
Planet formation by pebble accretion in ringed disks
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Most super-Earths formed by dry pebble accretion are less massive than 5 Earth masses
Aims. The goal of this work is to study the formation of rocky planets by dry pebble accretion from self-consistent dust-growth models. In particular, we aim to compute the maximum core mass of a
The eccentricity distribution of giant planets and their relation to super-Earths in the pebble accretion scenario
Observations of the population of cold Jupiter planets ($r>$1 AU) show that nearly all of these planets orbit their host star on eccentric orbits. For planets up to a few Jupiter masses, eccentric
The nature of the radius valley
The existence of a Radius Valley in the Kepler size distribution stands as one of the most important observational constraints to understand the origin and composition of exoplanets with radii
Probing the impact of varied migration and gas accretion rates for the formation of giant planets in the pebble accretion scenario
The final orbital position of growing planets is determined by their migration speed, which is essentially set by the planetary mass. Small mass planets migrate in type-I migration, while more
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Context. The origin of giant planets at moderate separations ≃1–10 au is still not fully understood because numerical studies of Type II migration in protoplanetary disks often predict a decay of the
From dust to planets – I. Planetesimal and embryo formation
  • G. Coleman
  • Physics, Geology
    Monthly Notices of the Royal Astronomical Society
  • 2021
Planet formation models begin with proto-embryos and planetesimals already fully formed, missing out a crucial step, the formation of planetesimals/proto-embryos. In this work, we include
The Nature and Origins of Sub‐Neptune Size Planets
TLDR
Results from NASA's Kepler mission have revealed a bimodality in the radius distribution of sub‐Neptune planets, with a relative underabundance of planets between 1.5 and 2.0 R⊕, which suggests that sub-Neptunes are mostly rocky planets that were born with primary atmospheres a few percent by mass accreted from the protoplanetary nebula.
Probing the Inner Edge of Dead Zones in Protoplanetary Disks with ALMA and Next Generation Very Large Array
The discovery of substructures in protoplanetary disks by the Atacama Large Millimeter/submillimeter Array (ALMA) has provided us with key insights into the formation of planets. However,
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