# Planets of β Pictoris revisited

@article{Freistetter2007PlanetsO,
title={Planets of $\beta$ Pictoris revisited},
author={Florian Freistetter and Alexander V. Krivov and Torsten Lohne Astrophysikalisches Institut and Friedrich-Schiller-Universitat Jena},
journal={Astronomy and Astrophysics},
year={2007},
volume={466},
pages={389-393}
}
• Published 2007
• Physics
• Astronomy and Astrophysics
Observations have revealed a large variety of structures (global asymmetries, warps, belts, rings) and dynamical phenomena (“falling-evaporating bodies” or FEBs, the “ β  Pic dust stream”) in the disk of β  Pictoris, most of which may indicate the presence of one or more planets orbiting the star. Because planets of β  Pic have not been detected by observations yet, we use dynamical simulations to find “numerical evidence” for a planetary system. We show that one planet at 12 AU with a mass of… Expand

#### Paper Mentions

Constraints on planets around β Pic with Harps radial velocity data
• Physics
• 2012
Context. The β Pictoris system with its debris disk and a massive giant planet orbiting at � 9 AU represents an ideal laboratory for studying giant planet formation and evolution as well asExpand
Planets in orbit around β Pictoris formed the orbital architecture of planetesimal belts?
We report near-infrared imaging observations of the β Pic dust disk, from which we infer the orbital architecture of planetesimal belts that remain near mean motion resonances (MMRs) with a planet atExpand
Orbital characterization of the β Pictoris b giant planet
In June 2010, we confirmed the existence of a giant planet in the disk of the young star Beta Pictoris, located between 8 AU and 15 AU from the star. This young planet offers the rare opportunity toExpand
A Giant Planet Imaged in the Disk of the Young Star β Pictoris
It is shown that the ~10-million-year-oldβ Pictoris system hosts a massive giant planet, β Pictoris b, located 8 to 15 astronomical units from the star, which confirms that gas giant planets form rapidly within disks and validates the use of disk structures as fingerprints of embedded planets. Expand
A probable giant planet imaged in the beta Pictoris disk. VLT/NaCo deep L'-band imaging
Context: Since the discovery of its dusty disk in 1984, β Pictoris has become the prototype of young early-type planetary systems, and there are now various indications that a massive Jovian planetExpand
ORBITAL CONSTRAINTS ON THE β Pic INNER PLANET CANDIDATE WITH KECK ADAPTIVE OPTICS
• Physics
• 2009
A point source observed 8 AU in projection from β Pictoris in L � (3.8 μm) imaging in 2003 has been recently presented as a planet candidate. Here we show the results of L � -band adaptive opticsExpand
Is Beta Pic b the transiting planet of November 1981
• Physics
• 2009
In 1981, Beta Pictoris showed strong and rapid photometric variations that were attributed to the transit of a giant comet or a planet orbiting at several AUs (Lecavelier des Etangs et al. 1994,Expand
Evolution of Debris Disks
Circumstellar dust exists around several hundred main sequence stars. For the youngest stars, that dust could be a remnant of the protoplanetary disk. Mostly it is inferred to be continuouslyExpand
The planet companion around β Pictoris
Abstract The β Pic disk of dust and gas has been regarded as the prototype of young planetary systems since the 1980s and has revealed over the years an impressive amount of indirect signs pointingExpand
Dynamics of Small Bodies in Planetary Systems
The number of stars that are known to have debris disks is greater than that of stars known to harbor planets. These disks are detected because dust is created in the destruction of planetesimals inExpand

#### References

SHOWING 1-10 OF 26 REFERENCES
Mid-infrared images of β Pictoris and the possible role of planetesimal collisions in the central disk
Thermal infrared images of the central disk imply that the brightness asymmetry results from the presence of a bright clump composed of particles that may differ in size from dust elsewhere in the disk, which is suggested to result from the collisional grinding of resonantly trapped planetesimals or the cataclysmic break-up of a planetesimal. Expand
Dynamical modeling of large scale asymmetries in the beta Pictoris dust disk
We report a new and complete model of the Pictoris disk, which succeeds in accounting for both the surface brightness distribution, warp characteristics, the outer \butterfly" asymmetry as observedExpand
Towards understanding the β Pictoris dust stream
• Physics
• 2004
The recent radar detection by Baggaley (2000) of a collimated stream of interstellar meteoroids postulated to be sourced at β Pictoris, a nearby star with a prominent dust disk, presents a challengeExpand
Falling Evaporating Bodies as a Clue to Outline the Structure of the β Pictoris Young Planetary System
• Physics
• 2000
Transient redshifted events monitored in the spectrum offl Pictoris have been interpreted for many years as resulting from the evaporation of numerous comet-like bodies in the vicinity of this stars.Expand
Mean-Motion Resonances as a Source for Infalling Comets toward β Pictoris
• Physics
• 1996
Abstract Repeated time-variable redshifted absorption features in the spectrum of β Pictoris (β Pic) have been attributed to comet-like bodies falling toward the star, when evaporating in itsExpand
Stellar Encounters with the β Pictoris Planetesimal System
• Physics
• 2001
We use data from the Hipparcos catalog and the Barbier-Brossat & Figon catalog of stellar radial velocities to test the hypothesis that the b Pic planetesimal disk was disrupted by a close stellarExpand
An early extrasolar planetary system revealed by planetesimal belts in β Pictoris
It is reported that the sub-micrometre amorphous silicate grains around β Pic have peaks in their distribution around 6, 16 and 30’au (1 au is the Sun–Earth distance), whereas the crystalline and micrometr-sized amorphously silicategrain grains are concentrated in the disk centre. Expand
The β Pictoris Moving Group
• Physics
• 2001
Following the 1983 IRAS detection and subsequent imaging of its extensive dusty circumstellar disk, β Pictoris became the prototypical and most studied example of a potential forming planetaryExpand
The Inner Rings of β Pictoris
• Physics
• 2003
We present Keck images of the dust disk around β Pictoris at λ = 17.9 μm that reveal new structure in its morphology. Within 1'' (19 AU) of the star, the long axis of the dust emission is rotated byExpand
Modeling the resonant planetary system GJ 876
• Physics
• 2005
The two planets about the star GJ 876 appear to have undergone extensive migration from their point of origin in the protoplanetary disk – both because of their close proximity to the star (30 and 60Expand