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

  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},
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
Context. Pebble accretion is expected to be the dominant process for the formation of massive solid planets, such as the cores of giant planets and super-Earths. So far, this process has been studied
Formation of planetary populations − II. Effects of initial disc size and radial dust drift
Recent ALMA observations indicate that while a range of disk sizes exist, typical disk radii are small, and that radial dust drift affects the distribution of solids in disks. Here we explore the
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
Migration of gap-opening planets in 3D stellar-irradiated accretion disks
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
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,


The structure of protoplanetary discs around evolving young stars
The formation of planets with gaseous envelopes takes place in protoplanetary accretion discs on time scales of several million years. Small dust particles stick to each other to form pebbles,
Many stars host planets orbiting within a few astronomical units (AU). The occurrence rate and distributions of masses and orbits vary greatly with the host stars mass. These close planets origins
Migration and the Formation of Systems of Hot Super-Earths and Neptunes
The existence of extrasolar planets with short orbital periods suggests that planetary migration induced by tidal interaction with the protoplanetary disk is important. Cores and terrestrial planets
A Lagrangian model for dust evolution in protoplanetary disks: formation of wet and dry planetesimals at different stellar masses
We introduce a new Lagrangian smooth-particle method to model the growth and drift of pebbles in protoplanetary disks. The Lagrangian nature of the model makes it especially suited to following
Planetesimal formation starts at the snow line
Planetesimal formation stage represents a major gap in our understanding of the planet formation process. The late-stage planet accretion models typically make arbitrary assumptions about
The effect of type I migration on the formation of terrestrial planets in hot-Jupiter systems
Context. Our previous models of a giant planet migrating through an inner protoplanet/planetesimal disk find that the giant shepherds a portion of the material it encounters into interior orbits,
Formation of short-period planets by disc migration
Protoplanetary discs are thought to be truncated at orbital periods of around 10 d. Therefore, the origin of rocky short-period planets with P < 10 d is a puzzle. We propose that many of these
Tidal evolution of close-in giant planets : Evidence of Type II migration?
It is well accepted that ‘hot Jupiters’ and other short-period planets did not form in situ, as the temperature in the protoplanetary disc at the radius at which they now orbit would have been too
Trapping Low-mass Planets at the Inner Edge of the Protostellar Disk
The formation of multiple close-in low-mass exoplanets is still a mystery. The challenge is to build a system wherein the outermost planet is beyond 0.2 AU from the star. Here we investigate how the
A simple model for the evolution of the dust population in protoplanetary disks
Context. The global size and spatial distribution of dust is an important ingredient in the structure and evolution of protoplanetary disks and in the formation of larger bodies, such as