Disc fragmentation rarely forms planetary-mass objects

@article{Rice2015DiscFR,
  title={Disc fragmentation rarely forms planetary-mass objects},
  author={Ken Rice and Eric D. Lopez and Duncan H. Forgan and Beth A. Biller},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2015},
  volume={454},
  pages={1940-1947}
}
  • K. RiceE. Lopez B. Biller
  • Published 26 August 2015
  • Environmental Science, Geology, Physics
  • Monthly Notices of the Royal Astronomical Society
KR gratefully acknowledges support from STFC grant ST/M001229/1. The research leading to these results also received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). DF grateful acknowledges support from the ECOGAL ERC advanced grant. 

Figures from this paper

Identifying and analysing protostellar disc fragments in smoothed particle hydrodynamics simulations

KR gratefully acknowledges support from STFC grant ST/M001229/1. DF gratefully acknowledges support from the ECOGAL project, grant agreement 291227, funded by the European Research Council under

Towards a population synthesis model of self-gravitating disc fragmentation and tidal downsizing II: the effect of fragment–fragment interactions

DHF gratefully acknowledges support from the ECOGAL project, grant agreement 291227, funded by the European Research Council (ERC) under ERC-2011-ADG. This project has received funding from ERC under

Characterizing gravito-turbulence in 3D: turbulent properties and stability against fragmentation

This work has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC-2013-ADG and has used the DIRAC Shared Memory Processing and DiRAC Data

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits. IV. Gravitational instability rarely forms wide, giant planets

Understanding the formation and evolution of giant planets (≥1 M_(Jup)) at wide orbital separation (≥5 AU) is one of the goals of direct imaging. Over the past 15 yr, many surveys have placed strong

Giant planet migration during FU Orionis outbursts: 1D disc models

I present the results of semi-analytic calculations of migrating planets in young, outbursting circumstellar discs. Formed far out in the disc via gravitational fragmentation early on in its

Fragmentation of Kozai–Lidov Disks

We analyze the gravitational instability (GI) of a locally isothermal inclined disk around one component of a binary system. Such a disk can undergo global Kozai–Lidov (KL) cycles if the initial disk

On the Diversity in Mass and Orbital Radius of Giant Planets Formed via Disk Instability

We present a semi-analytical population synthesis model of protoplanetary clumps formed by disk instability at radial distances of 80–120 au. Various clump density profiles, initial mass functions,

Giant planets and brown dwarfs on wide orbits: a code comparison project

Gas clumps formed within massive gravitationally unstable circumstellar discs are potential seeds of gas giant planets, brown dwarfs, and companion stars. Competition between three processes –

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

Stellar multiplicity is believed to influence planetary formation and evolution, although the precise nature and extent of this role remain ambiguous. We present a study aimed at testing the role

The Effect of Protoplanetary Disk Cooling Times on the Formation of Gas Giant Planets by Gravitational Instability

Observational evidence exists for the formation of gas giant planets on wide orbits around young stars by disk gravitational instability, but the roles of disk instability and core accretion for

References

SHOWING 1-10 OF 88 REFERENCES

The dynamical fate of self-gravitating disc fragments after tidal downsizing

DF and KR acknowledge support from STFC grant ST/J001422/1. DF also acknowledges support from the ECOGAL ERC Advanced Grant Programme. RJP acknowledges support from the Royal Astronomical Society in

STEADY-STATE PLANET MIGRATION BY THE KOZAI–LIDOV MECHANISM IN STELLAR BINARIES

We study the steady-state orbital distributions of giant planets migrating through the combination of the Kozai–Lidov (KL) mechanism due to a stellar companion and friction due to tides raised on the

FRAGMENT PRODUCTION AND SURVIVAL IN IRRADIATED DISKS: A COMPREHENSIVE COOLING CRITERION

Accretion disks that become gravitationally unstable can fragment into stellar or substellar companions. The formation and survival of these fragments depends on the precarious balance between

Positive metallicity correlation for coreless giant planets

Frequency of detected giant planets is observed to increase rapidly with metallicity of the host star. This is usually interpreted as evidence in support of the core accretion (CA) theory, which

The Planet-Metallicity Correlation

We have recently carried out spectral synthesis modeling to determine Teff, log g, v sin i, and [Fe/H] for 1040 FGK-type stars on the Keck, Lick, and Anglo-Australian Telescope planet search

Rapid inward migration of planets formed by gravitational instability

The observation of massive exoplanets at large separation (10 au) from their host star, like in the HR 8799 system, challenges theories of planet formation. A possible formation mechanism involves

Planet Migration and Binary Companions: The Case of HD 80606b

The exosolar planet HD 80606b has a highly eccentric (e = 0.93) and tight (a = 0.47 AU) orbit. We study how it might arrive at such an orbit and how it has avoided being tidally circularized until

THE PHOTOECCENTRIC EFFECT AND PROTO-HOT JUPITERS. III. A PAUCITY OF PROTO-HOT JUPITERS ON SUPER-ECCENTRIC ORBITS

Gas giant planets orbiting within 0.1 AU of their host stars are unlikely to have formed in situ and are evidence for planetary migration. It is debated whether the typical hot Jupiter smoothly

The minimum mass for star formation, and the origin of binary brown dwarfs

Context. The minimum mass for star formation is a critical parameter with profound astrophysical, cosmological and anthropic consequences. Aims. Our first aim is to calculate the minimum mass for

THE SIGNATURE OF THE ICE LINE AND MODEST TYPE I MIGRATION IN THE OBSERVED EXOPLANET MASS–SEMIMAJOR AXIS DISTRIBUTION

Existing exoplanet radial velocity surveys are complete in the planetary mass–semimajor axis (Mp–a) plane over the range 0.1 AU <a< 2.0 AU where Mp ≳ 100 M⊕. We marginalize over mass in this complete
...