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…
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References
SHOWING 1-10 OF 80 REFERENCES
The structure of protoplanetary discs around evolving young stars
- Geology, Physics
- 2014
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,…
RADIATION HYDRODYNAMICS MODELS OF THE INNER RIM IN PROTOPLANETARY DISKS
- Physics, Geology
- 2016
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
- Geology, Physics
- 2007
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
- Physics, GeologyAstronomy & Astrophysics
- 2018
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
- Physics, Geology
- 2017
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
- Geology, Physics
- 2007
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
- Geology, PhysicsMonthly Notices of the Royal Astronomical Society
- 2019
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?
- Geology, Physics
- 2012
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
- Physics, GeologyThe Astrophysical Journal
- 2018
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
- Geology, Physics
- 2012
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…