The mass of the young planet Beta Pictoris b through the astrometric motion of its host star

  title={The mass of the young planet Beta Pictoris b through the astrometric motion of its host star},
  author={Ignas A. G. Snellen and Anthony G. A. Brown},
  journal={Nature Astronomy},
The young massive Jupiters discovered with high-contrast imaging1–4 provide a unique opportunity to study the formation and early evolution of gas giant planets. A key question is to what extent gravitational energy from accreted gas contributes to the internal energy of a newly formed planet. This has led to a range of formation scenarios from ‘cold’ to ‘hot’ start models5–8. For a planet of a given mass, these initial conditions govern its subsequent evolution in luminosity and radius. Except… 
Evidence for an additional planet in the β Pictoris system
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CO Detected in CI Tau b: Hot Start Implied by Planet Mass and MK
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A planet within the debris disk around the pre-main sequence star AU Mic
The authors' observations of a planet co-existing with a debris disk offer the opportunity to test the predictions of current models of planet formation and evolution, and a transiting planet with a period of about 8.5 days and a radius 0.4 times that of Jupiter is reported within the debris disk around the star AU Microscopii.
Precise Dynamical Masses of Directly Imaged Companions from Relative Astrometry, Radial Velocities, and Hipparcos–Gaia DR2 Accelerations
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The far reaches of the β Pictoris debris disk
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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.
On the Luminosity of Young Jupiters
Traditional thermal evolution models of giant planets employ arbitrary initial conditions selected more for computational expediency than physical accuracy. Since the initial conditions are
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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 planet
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Full exploration of the giant planet population around β Pictoris
Context. The search for extrasolar planets has been limited so far to close orbit (typ. ≤5 au) planets around mature solar-type stars on the one hand, and to planets on wide orbits (≥10 au) around
Gas-giant planets that form via core accretion might have very different characteristics from those that form via disk instability. Disk-instability objects are typically thought to have higher
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High-contrast observations with the Keck and Gemini telescopes have revealed three planets orbiting the star HR 8799, with projected separations of 24, 38, and 68 astronomical units.
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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 planetary