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… 
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
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
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 Effect of a Strong Pressure Bump in the Sun’s Natal Disk: Terrestrial Planet Formation via Planetesimal Accretion Rather than Pebble Accretion
Mass-independent isotopic anomalies of carbonaceous and noncarbonaceous meteorites show a clear dichotomy suggesting an efficient separation of the inner and outer solar system. Observations show
Drifting inwards in protoplanetary discs I Sticking of chondritic dust at increasing temperatures
Sticking properties rule the early phases of pebble growth in protoplanetary discs in which grains regularly travel from cold, water-rich regions to the warm inner part. This drift affects
TOI-216: Resonant Constraints on Planet Migration
TOI-216 is a pair of close-in planets with orbits deep in the 2:1 mean motion resonance. The inner Neptune-class planet (TOI-216b) is near 0.12 au (orbital period P b ≃ 17 days) and has a substantial
The origins of nearly coplanar, non-resonant systems of close-in super-Earths
Some systems of close-in "super-Earths" contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of this class of system.
The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
In 2017, the California-Kepler Survey (CKS) published its first data release (DR1) of high-resolution optical spectra of 1305 planet hosts. Refined CKS planet radii revealed that small planets are
Planet Formation
The CARMENES search for exoplanets around M dwarfs
We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, mb = 30.8 ± 1.5M⊕, Rb = 4.7 ± 0.3 R⊕) located in the “hot Neptune desert”. Confirmation of the TESS Object of Interest


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
Formation of planetary systems by pebble accretion and migration
At least 30% of main sequence stars host planets with sizes between 1 and 4 Earth radii and orbital periods of less than 100 days. We use N-body simulations including a model for gas-assisted pebble
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