In Situ and Ex Situ Formation Models of Kepler 11 Planets

@article{dAngelo2016InSA,
  title={In Situ and Ex Situ Formation Models of Kepler 11 Planets},
  author={G. d'Angelo and P. Bodenheimer},
  journal={arXiv: Earth and Planetary Astrophysics},
  year={2016}
}
We present formation simulations of the six Kepler 11 planets. Models assume either in situ or ex situ assembly, the latter with migration, and are evolved to the estimated age of the system, 8 Gyr. Models combine detailed calculations of both the gaseous envelope and the condensed core structures, including accretion of gas and solids, of the disk's viscous and thermal evolution, including photo-evaporation and disk-planet interactions, and of the planets' evaporative mass loss after disk… Expand
New Formation Models for the Kepler-36 System
Formation of the planets in the Kepler-36 system is modeled by detailed numerical simulations according to the core-nucleated accretion scenario. The standard model is updated to include theExpand
Super-Earths: Atmospheric Accretion, Thermal Evolution and Envelope Loss
Combined mass and radius observations have recently revealed many short-period planets a few times the size of Earth but with significantly lower densities. A natural explanation for the low densityExpand
Formation of Giant Planets
Giant planets are tens to thousands of times as massive as the Earth, and many times as large. Most of their volumes are occupied by hydrogen and helium, the primary constituents of the protostellarExpand
An Analytic Criterion for Turbulent Disruption of Planetary Resonances
Mean motion commensurabilities in multi-planet systems are an expected outcome of protoplanetary disk-driven migration, and their relative dearth in the observational data presents an importantExpand
Three Super-Earths Transiting the Nearby Star GJ 9827
We report on the discovery of three transiting planets around GJ 9827. The planets have radii of 1.75 ± 0.18, 1.36 ± 0.14, and 2.11_-0.21^+0.22 R⊕, and periods of 1.20896, 3.6480, and 6.2014 days,Expand
Yarkovsky and YORP Effects in Dynamics of Small Bodies of the Solar System
In this thesis, we study the influence of non-gravitational perturbations induced by the Yarkovsky/YORP effect and solar radiation pressure (SRP) on the orbital evolution of selected asteroids,Expand
Factoring Origin of Life Hypotheses into the Search for Life in the Solar System and Beyond
TLDR
The relative probability that life could have emerged in environments on early Mars, on the icy moons of Jupiter and Saturn, and also the degree to which prebiotic chemistry could have advanced on Titan are discussed. Expand
The dehydration of water worlds via atmospheric losses
We present a three-species multi-fluid MHD model (H$^+$, H$_2$O$^+$ and e$^-$), endowed with the requisite atmospheric chemistry, that is capable of accurately quantifying the magnitude of water ionExpand
Growth of Jupiter: Formation in disks of gas and solids and evolution to the present epoch
Abstract The formation of Jupiter is modeled via core-nucleated accretion, and the planet's evolution is simulated up to the present epoch. Throughout the phases when the planet acquires most of theExpand

References

SHOWING 1-10 OF 174 REFERENCES
Models of the in Situ Formation of Detected Extrasolar Giant Planets
Abstract We present numerical simulations of the formation of the planetary companions to 47 UMa, ρ CrB, and 51 Peg. They are assumed to have formed in situ according to the basic model that a coreExpand
Accretion and Evolution of ~2.5 Earth-mass Planets with Voluminous H/He Envelopes
Formation of planets in the Neptune size range with low-mass, but voluminous, H_2/He gaseous envelopes is modeled by detailed numerical simulations according to the core-nucleated accretion scenario.Expand
Formation of the Giant Planets by Concurrent Accretion of Solids and Gas
New numerical simulations of the formation of the giant of the second phase. planets are presented, in which for the first time both the gas and The actual rates at which the giant planets accretedExpand
Formation of the giant planets
Observational constraints on interior models of the giant planets indicate that these planets were all much hotter when they formed and they all have rock and/or ice cores of ten to thirty earthExpand
TESTING IN SITU ASSEMBLY WITH THE KEPLER PLANET CANDIDATE SAMPLE
We present a Monte Carlo model for the structure of low-mass (total mass <25 M ?) planetary systems that form by the in situ gravitational assembly of planetary embryos into final planets. Our modelExpand
Evolution of Migrating Planets Undergoing Gas Accretion
We analyze the orbital and mass evolution of planets that undergo runaway gas accretion by means of two- and three-dimensional hydrodynamic simulations. The disk torque distribution per unit diskExpand
A reassessment of the in situ formation of close-in super-Earths
Context. A large fraction of stars host one or multiple close-in super-Earth planets. There is an active debate about whether these planets formed in situ or at greater distances from the centralExpand
Mass–radius curve for extrasolar Earth-like planets and ocean planets
Abstract By comparison with the Earth-like planets and the large icy satellites of the Solar System, one can model the internal structure of extrasolar planets. The input parameters are theExpand
Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets
In an attempt to develop a deterministic theory for planet formation, we examine the accretion of cores of giant planets from planetesimals, gas accretion onto the cores, and their orbital migration.Expand
Towards a Deterministic Model of Planetary Formation I : a Desert in the Mass and Semi Major Axis Distributions of Extra Solar Planets
In an attempt to develop a deterministic theory for planet formation, we examine the accretion of cores of giant planets from planetesimals, gas accretion onto the cores, and their orbital migration.Expand
...
1
2
3
4
5
...