Fast spin of the young extrasolar planet β Pictoris b

@article{Snellen2014FastSO,
  title={Fast spin of the young extrasolar planet $\beta$ Pictoris b},
  author={Ignas A. G. Snellen and Bernhard Brandl and Remco J. de Kok and Matteo Brogi and Jayne L. Birkby and Henriette Schwarz},
  journal={Nature},
  year={2014},
  volume={509},
  pages={63-65}
}
The spin of a planet arises from the accretion of angular momentum during its formation, but the details of this process are still unclear. In the Solar System, the equatorial rotation velocities and, consequently, spin angular momenta of most of the planets increase with planetary mass; the exceptions to this trend are Mercury and Venus, which, since formation, have significantly spun down because of tidal interactions. Here we report near-infrared spectroscopic observations, at a resolving… 
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References

SHOWING 1-10 OF 60 REFERENCES
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 to
The signature of orbital motion from the dayside of the planet τ Boötis b
TLDR
The detection of carbon monoxide absorption in the thermal dayside spectrum of τ Boötis b supports the hypothesis that the absorbing compounds believed to cause such atmospheric inversions are destroyed in τ Bo Ötis b by the ultraviolet emission from the active host star.
A Giant Planet Imaged in the Disk of the Young Star β Pictoris
TLDR
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.
Beta Pictoris light variations. I. The planetary hypothesis
The Pic disk is probably a young planetary system in the clearing-out phase and similar to ours 4 billion years ago. The understanding of that system may shed light on the origin and evolution of our
On the Origin of Planetary Spins
Abstract We examine the rate of accretion of mass and spin angular momentum by a spherical solid body ("planet") immersed in a differentially rotating disk of particles ("planetesimals"). If the
The four final rotation states of Venus
TLDR
Here it is shown that independent of uncertainties in the models, terrestrial planets with dense atmosphere like Venus can evolve into one of only four possible rotation states, and that most initial conditions will drive the planet towards the configuration at present seen at Venus, albeit through two very different evolutionary paths.
The near-infrared spectral energy distribution of β Pictoris b
A gas giant planet has previously been directly seen orbiting at 8-10 AU within the debris disk of the ~12 Myr old star {\beta} Pictoris. The {\beta} Pictoris system offers the rare opportunity to
Prograde rotation of protoplanets by accretion of pebbles in a gaseous environment
We perform hydrodynamical simulations of the accretion of pebbles and rocks on to protoplanets of a few hundred kilometres in radius, including two-way drag force coupling between particles and the
Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458
We present evolutionary models for cool brown dwarfs and extra-solar giant planets. The models re- produce the main trends of observed methane dwarfs in near-IR color-magnitude diagrams. We also
...
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