Migration and the Formation of Systems of Hot Super-Earths and Neptunes

  title={Migration and the Formation of Systems of Hot Super-Earths and Neptunes},
  author={Caroline Terquem and John C. B. Papaloizou},
  journal={The Astrophysical Journal},
  pages={1110 - 1120}
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 may undergo migration as they form. In this paper we investigate the evolution of a population of cores with initial masses in the range 0.1-1 M⊕ embedded in a disk. Mutual interactions lead to orbit crossing and mergers, so that the cores grow during their evolution. Interaction with the disk leads… 

Figures and Tables from this paper

Dynamical rearrangement of super-Earths during disk dispersal - I. Outline of the magnetospheric rebound model
Context. The Kepler mission has discovered that close-in super-Earth planets are common around solar-type stars. They are often seen together in multiplanetary systems, but their period ratios do not
Formation of planetary systems by pebble accretion and migration
At least 30% of main sequence stars host planets with sizes of 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
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
Planet formation and migration near the silicate sublimation front in protoplanetary disks
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
Hot super-Earths and giant planet cores from different migration histories
Planetary embryos embedded in gaseous protoplanetary disks undergo Type I orbital migration. Migration can be inward or outward depending on the local disk properties but, in general, only planets
I explore whether close-in super-Earths were formed as rocky bodies that failed to grow fast enough to become the cores of gas giants before the natal protostellar disk dispersed. I model the failed
The recent Kepler discovery of KOI-152 reveals a system of three hot super-Earth candidates that are in or near a 4:2:1 mean motion resonance. It is unlikely that they formed in situ; the planets
Dynamical rearrangement of super-Earths during disk dispersal II. Assessment of the magnetospheric rebound model for planet formation scenarios
Context.The Kepler mission has provided a large sample to statistically analyze the orbital properties of the super-Earth planets. We hypothesize that these planets formed early and consider the
Evolution of the eccentricity and orbital inclination caused by planet-disc interactions
Since the discovery of the first planet orbiting a main-sequence star outside the solar system in 1995, the field of exoplanet studies has grown rapidly, both from the observational and theoretical
On the formation of planetary systems in photoevaporating transition discs
In protoplanetary discs, planetary cores must be at least 0.1 earth mass at 1 au for migration to be significant; this mass rises to 1 earth mass at 5 au. Planet formation models indicate that these


Dynamical relaxation and massive extrasolar planets
Following the suggestion of Black that some massive extrasolar planets may be associated with the tail of the distribution of stellar companions, we investigate a scenario in which 5 < N < 100
On disc driven inward migration of resonantly coupled planets with application to the system around GJ876
We consider two protoplanets gravitationally interacting with each other and a protoplanetary disc. The two planets orbit interior to a tidally maintained disc cavity while the disc interaction
On the migration-induced resonances in a system of two planets with masses in the Earth mass range
We investigate orbital resonances expected to arise when a system of two planets, with masses in the range 1–4 M⊕, undergoes convergent migration while embedded in a section of gaseous disc where the
Effects of Type I Migration on Terrestrial Planet Formation
Planetary embryos embedded in a gas disk suffer a decay in semimajor axis—type I migration—due to the asymmetric torques produced by the interior and exterior wakes raised by the body. This presents
On the migration of a system of protoplanets
ABSTRA C T The evolution of a system consisting of a protoplanetary disc with two embedded Jupitersized planets is studied numerically. The disc is assumed to be flat and non-self-gravitating; this
The interaction of giant planets with a disc with MHD turbulence – IV. Migration rates of embedded protoplanets
We present the results of global cylindrical disc simulations and local shearing box simulations of protoplanets interacting with a disc undergoing magnetohydrodynamic (MHD) turbulence. The specific
Reversing type II migration: resonance trapping of a lighter giant protoplanet
We present new results related to the coupled evolution of a two giant planet system embedded in a protoplanetary disk, in which a Saturn mass protoplanet is trapped in an outer mean motion resonance
On the orbital evolution and growth of protoplanets embedded in a gaseous disc
ABSTRA C T We present a new computation of the linear tidal interaction of a protoplanetary core with a thin gaseous disc in which it is fully embedded. For the first time a discussion of the orbital
On the evolution of multiple protoplanets embedded in a protostellar disc
Context. Theory predicts that low mass protoplanets in a laminar protostellar disc will migrate into the central star prior to disc dispersal. It is known that protoplanets on orbits with