Fast spin of the young extrasolar planet β Pictoris b

Snellen, I. A. G.; Brandl, Bernhard R.; Kok, Remco de; Brogi, Matteo; Birkby, Jayne; Schwarz, H.

doi:10.1038/nature13253

Cited by 410 publications

(446 citation statements)

References 37 publications

Supporting

Mentioning

427

Contrasting

Order By: Relevance

“…An even higher value may be expected at longer wavelengths. Such signals should be easily detectable with recent instruments such as SPHERE or using a detailed spectroscopic analysis (Brogi et al 2012;Snellen et al 2014;Martins et al 2015). We note that the projected distance on the sky between the star and the planet is about 0.14 arcsec at apastron.…”

Section: A System Full Of Potentialmentioning

confidence: 83%

An extreme planetary system around HD 219828

Santos

Santerne

Faria

et al. 2016

A&A

View full text Add to dashboard Cite

Context. With about 2000 extrasolar planets confirmed, the results show that planetary systems have a whole range of unexpected properties. This wide diversity provides fundamental clues to the processes of planet formation and evolution. Aims. We present a full investigation of the HD 219828 system, a bright metal-rich star for which a hot Neptune has previously been detected. Methods. We used a set of HARPS, SOPHIE, and ELODIE radial velocities to search for the existence of orbiting companions to HD 219828. The spectra were used to characterise the star and its chemical abundances, as well as to check for spurious, activity induced signals. A dynamical analysis is also performed to study the stability of the system and to constrain the orbital parameters and planet masses. Results. We announce the discovery of a long period (P = 13.1 yr) massive (m sin i = 15.1 M Jup ) companion (HD 219828 c) in a very eccentric orbit (e = 0.81). The same data confirms the existence of a hot Neptune, HD 219828 b, with a minimum mass of 21 M ⊕ and a period of 3.83 days. The dynamical analysis shows that the system is stable, and that the equilibrium eccentricity of planet b is close to zero. Conclusions. The HD 219828 system is extreme and unique in several aspects. First, ammong all known exoplanet systems it presents an unusually high mass ratio. We also show that systems like HD 219828, with a hot Neptune and a long-period massive companion are more frequent than similar systems with a hot Jupiter instead. This suggests that the formation of hot Neptunes follows a different path than the formation of their hot jovian counterparts. The high mass, long period, and eccentricity of HD 219828 c also make it a good target for Gaia astrometry as well as a potential target for atmospheric characterisation, using direct imaging or high-resolution spectroscopy. Astrometric observations will allow us to derive its real mass and orbital configuration. If a transit of HD 219828 b is detected, we will be able to fully characterise the system, including the relative orbital inclinations. With a clearly known mass, HD 219828 c may become a benchmark object for the range in between giant planets and brown dwarfs.

show abstract

Section: A System Full Of Potentialmentioning

confidence: 83%

An extreme planetary system around HD 219828

Santos

Santerne

Faria

et al. 2016

A&A

View full text Add to dashboard Cite

show abstract

“…Subsequent direct and coronagraphic imaging of the planet (Currie et al 2013;Morzinski et al 2015) shows that the planet's projected separation is decreasing, with the orbit almost edge on to our line of sight. Radial velocity measurements by Snellen et al (2014) show that the planet's projected velocity is blue shifted, and that the planet is moving towards inferior conjunction. Astrometric monitoring indicates a period of approximately 20 yr for the planet's orbit (Chauvin et al 2012;Nielsen et al 2014;Millar-Blanchaer et al 2015).…”

Section: β Pictoris B and The Inferior Conjunction Of 2017mentioning

confidence: 99%

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

Stuik

Bailey

Dorval

et al. 2017

A&A

View full text Add to dashboard Cite

Aims. We describe the design and first light observations from the β Pictoris b Ring ("bRing") project. The primary goal is to detect photometric variability from the young star β Pictoris due to circumplanetary material surrounding the directly imaged young extrasolar gas giant planet β Pictoris b. Methods. Over a nine month period centred on September 2017, the Hill sphere of the planet will cross in front of the star, providing a unique opportunity to directly probe the circumplanetary environment of a directly imaged planet through photometric and spectroscopic variations. We have built and installed the first of two bRing monitoring stations (one in South Africa and the other in Australia) that will measure the flux of β Pictoris, with a photometric precision of 0.5% over 5 min. Each station uses two wide field cameras to cover the declination of the star at all elevations. Detection of photometric fluctuations will trigger spectroscopic observations with large aperture telescopes in order to determine the gas and dust composition in a system at the end of the planet-forming era. Results. The first three months of operation demonstrate that bRing can obtain better than 0.5% photometry on β Pictoris in five minutes and is sensitive to nightly trends enabling the detection of any transiting material within the Hill sphere of the exoplanet.

show abstract

“…In some cases this can be significant, perhaps explaining the tilt of Uranus' spin relative to its orbital plane. Exoplanet spins are already measurable in observations of the velocity profile from lines in their atmospheres (Snellen et al 2014). For now such observations have been applied to one of the most massive known extrasolar planets (∼ 8M jup β Pic-b), showing it to spin much faster than its Solar System counterparts, likely due to its higher mass as opposed to its collisional history.…”

Section: Giant Impact Extrasolar Observablesmentioning

confidence: 99%

Insights into Planet Formation from Debris Disks

Wyatt

Jackson

2016

Space Sci Rev

View full text Add to dashboard Cite

Giant impacts refer to collisions between two objects each of which is massive enough to be considered at least a planetary embryo. The putative collision suffered by the proto-Earth that created the Moon is a prime example, though most Solar System bodies bear signatures of such collisions. Current planet formation models predict that an epoch of giant impacts may be inevitable, and observations of debris around other stars are providing mounting evidence that giant impacts feature in the evolution of many planetary systems. This chapter reviews giant impacts, focussing on what we can learn about planet formation by studying debris around other stars. Giant impact debris evolves through mutual collisions and dynamical interactions with planets. General aspects of this evolution are outlined, noting the importance of the collision-point geometry. The detectability of the debris is discussed using the example of the Moon-forming impact. Such debris could be detectable around another star up to 10 Myr post-impact, but model uncertainties could reduce detectability to a few 100 yr window. Nevertheless the 3 % of young stars with debris at levels expected during terrestrial planet formation provide valuable constraints on formation models; implications for super-Earth formation are also discussed. Variability recently observed in some bright disks promises to illuminate the evolution during the earliest phases when vapour condensates may be optically thick and acutely affected by the collision-point geometry. The outer reaches of planetary systems may also exhibit signatures of giant impacts, such as the clumpy debris structures seen around some stars.

show abstract

Fast spin of the young extrasolar planet β Pictoris b

Cited by 410 publications

References 37 publications

An extreme planetary system around HD 219828

An extreme planetary system around HD 219828

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

Insights into Planet Formation from Debris Disks

Contact Info

Product

Resources

About