Spin–Orbit Alignment of the β Pictoris Planetary System

  title={Spin–Orbit Alignment of the $\beta$ Pictoris Planetary System},
  author={Stefan Kraus and Jean-Baptiste Le Bouquin and Alexander Kreplin and Claire L. Davies and Edward Hone and John D. Monnier and Tyler Gardner and Grant M. Kennedy and Sasha Hinkley},
  journal={arXiv: Earth and Planetary Astrophysics},
A crucial diagnostic that can tell us about processes involved in the formation and dynamical evolutionof planetary systems is the angle between the rotation axis of a star and a planet's orbital angular momentum vector ("spin-orbit" alignment or "obliquity"). Here we present the first spin-orbit alignment measurement for a wide-separation exoplanetary system, namely on the directly-imaged planet $\beta$ Pictoris b. We use VLTI/GRAVITY spectro-interferometry with an astrometric accuracy of 1… 

Figures from this paper

Mutual inclinations between giant planets and their debris discs in HD 113337 and HD 38529
HD 113337 and HD 38529 host pairs of giant planets, a debris disc, and wide M-type stellar companions. We measure the disc orientation with resolved images from Herschel and constrain the
TOI-942b: A Prograde Neptune in a ∼ 60 Myr Old Multi-transiting System
Mapping the orbital obliquity distribution of young planets is one avenue toward understanding mechanisms that sculpt the architectures of planetary systems. TOI-942 is a young field star, with an
A Disk-driven Resonance as the Origin of High Inclinations of Close-in Planets
The recent characterization of transiting close-in planets has revealed an intriguing population of sub-Neptunes with highly tilted and even polar orbits relative to their host star's equator. Any
Direct confirmation of the radial-velocity planetβPictoris c
Context.Methods used to detect giant exoplanets can be broadly divided into two categories: indirect and direct. Indirect methods are more sensitive to planets with a small orbital period, whereas
Star and planet formation with the new generation VLTI and CHARA beam combiners
The diversity of planetary systems discovered in recent years has reinforced the interest in the conditions of the formation of stars and their planetary systems. The new generation of imaging
The β Pictoris b Hill sphere transit campaign
Aims. Photometric monitoring of β Pic in 1981 showed anomalous fluctuations of up to 4% over several days, consistent with foreground material transiting the stellar disk. The subsequent discovery of
Precise Dynamical Masses and Orbital Fits for β Pic b and β Pic c
We present a comprehensive orbital analysis to the exoplanets β Pictoris b and c that resolves previously reported tensions between the dynamical and evolutionary mass constraints on β Pic b. We use
A triple-star system with a misaligned and warped circumstellar disk shaped by disk tearing
Observations of the triple-star system GW Orionis are presented, finding evidence for disk tearing, which could provide a mechanism for forming wide-separation planets on oblique orbits.
Integral Field Spectroscopy with the Solar Gravitational Lens
The prospect of combining integral field spectroscopy with the solar gravitational lens (SGL) to spectrally and spatially resolve the surfaces and atmospheres of extrasolar planets is investigated.
On the Detection of Exomoons Transiting Isolated Planetary-mass Objects
All-sky imaging surveys have identified several dozen isolated planetary-mass objects (IPMOs) far away from any star. Here we examine the prospects for detecting transiting moons around these


Evolution of spin direction of accreting magnetic protostars and spin–orbit misalignment in exoplanetary systems
Recent observations have shown that in many exoplanetary systems the spin axis of the parent star is misaligned with the planet’s orbital axis. These have been used to argue against the scenario that
The spin-orbit alignment of the Fomalhaut planetary system probed by optical long baseline interferometry
Aims. We discuss the spin-orbit orientation of the Fomalhaut planetary system composed of a central A4V star, a debris disk, and a recently discovered planetary companion. Methods. We use spectrally
Evidence for an additional planet in the β Pictoris system
With its imaged debris disk of dust, its evaporating exocomets, and an imaged giant planet, the young (~23 Myr) β Pictoris system is a unique proxy for detailed studies of planet formation processes
On the Misalignment of the Directly Imaged Planet β Pictoris b with the System's Warped Inner Disk
The vertical warp in the debris disk β Pictoris—an inclined inner disk extending into a flat outer disk—has long been interpreted as the signpost of a planet on an inclined orbit. Direct images
The position of β Pictoris b position relative to the debris disk
Context. We detected in 2009 a giant, close-by planet orbiting β Pic, a young star surrounded by a disk that has been extensively studied for more than 20 years. We showed that if the planet were
The mass of the young planet Beta Pictoris b through the astrometric motion of its host star
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
© 2015. The American Astronomical Society. All rights reserved. We present H-band observations of β Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between
Peering into the formation history of β Pictoris b with VLTI/GRAVITY long-baseline interferometry
Context. β Pictoris is arguably one of the most studied stellar systems outside of our own. Some 30 yr of observations have revealed a highly-structured circumstellar disk, with rings, belts, and a
Shrinking binary and planetary orbits by Kozai cycles with tidal friction
At least two arguments suggest that the orbits of a large fraction of binary stars and extrasolar planets shrank by 1-2 orders of magnitude after formation: (1) the physical radius of a star shrinks
Constraining the orbit of the possible companion to Beta Pictoris: New deep imaging observations
We recently reported on the detection of a possible planetary-mass companion to Beta Pictoris at a projected separation of 8 AU from the star, using data taken in November 2003 with NaCo, the