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Newborn Giant Planet Grazes its Sun

Par Jean-Francois Donati - 20/06/2016

 

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Newborn Giant Planet Grazes its Sun

For the last 20 years the giant planets known as hot Jupiters have presented astronomers with a puzzle. How did they settle into orbits 100 times closer to their host stars than our own Jupiter is to the Sun ? An international team of astronomers has announced this week1 the discovery of a newborn hot Jupiter, orbiting an infant sun - only 2 million years old, the stellar equivalent of a week-old human baby. The discovery that hot Jupiters can already be present at such an early stage of star-planet formation represents a major step forward in our understanding of how planetary systems form and evolve.

For this discovery, the team monitored a 2 million-year-old infant star called V830 Tau, located in the Taurus stellar nursery, some 430 light-years away. Over the 1.5 months of the campaign, a regular 4.9-day “wobble” in the velocity of the host star revealed a giant planet almost as massive as Jupiter, orbiting its host star at a distance of only one-twentieth that of the Sun to the Earth distance. « Our discovery demonstrates for the first time that such bodies can be generated at very early stages of planetary formation, and likely play a central role in shaping the overall architecture of planetary systems » explains Jean-François Donati, CNRS astronomer at IRAP / OMP2 and lead author of a new paper in the current issue of the journal Nature.

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Artist view of a newborn giant planet like the one newly discovered at the immediate vicinity of the very active infant star V830 Tau, as seen by an observer located close to the giant planet (credit Mark A. Garlick / markgarlick.com)

In our Solar System, small rocky planets like the Earth are found near the Sun, whereas gas giants like Jupiter and Saturn orbit much further out. « The discovery in 1995 of a giant planet flying very close to its host star took us by surprise and revolutionized the field » recalls Claire Moutou, CNRS astronomer at the Canada-France-Hawaii Telescope3 (CFHT) and a coauthor of this new study. Theoretical work indicates that such planets can only form in the cold and icy outer regions of the protoplanetary disc in which both the central star and surrounding planets are born. Some, however, migrate inwards without falling into their host star, thus becoming hot Jupiters.

« Planet formation models offer two competing explanations of how and when this migration of hot Jupiters occurred. Either it happened early while these planets were still forming, or much later, with some planets being kicked closer to their stars due to the interaction of multiple planets, or both » explains Clément Baruteau, CNRS astronomer at IRAP / OMP and a coauthor of this study. « Our discovery demonstrates that the first, earlier option is taking place ; it revives the long-running debate about how and when this migration occurs, and brings us one step forward in our understanding of how planetary systems form ».

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The youngest known hot Jupiter discovered around the active young sun V830 Tau flies in the inner magnetic web of its host star (blue/white lines for open/closed field) as observed with spectropolarimetry and reconstructed using tomographic techniques inspired from medical imaging (credit JF Donati)

Among the known hot Jupiters, some feature strongly-tilted or even upside-down orbits, suggesting they were knocked into close orbits by interactions with other planets or neighboring stars. Others orbit above the host star’s equator, hinting at a more gentle formation process in the form of an inward drift through the disc. « The young hot Jupiter we just detected comes as the first evidence that early disc migration is also happening » says Andrew Collier Cameron of the University of St Andrews, a coauthor of the study.

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Brightness and magnetic spots at the surfaces of V830 Tau induce spectral perturbations much larger than those caused by the reflex motion of the detected giant planet. This animation illustrates the line profile distortions and associated spectral shifts (scaled up by 20x) induced by activity (blue arrow), by the detected planet (green) and by both (red) on the spectrum of V830 Tau (credit JF Donati).

For this discovery, the team used the twin spectropolarimeters ESPaDOnS and Narval, built at IRAP / OMP in Toulouse, France. ESPaDOnS is mounted at the 3.6-m CFHT on Maunakea, a dormant volcano on the Big Island of Hawaii, and can be fibre-fed from either CFHT itself, or via GRACES, a 300-m optical-fibre link from the nearby 8-m Gemini North telescope, with both modes used for our study. Narval is mounted at the 2-m Télescope Bernard Lyot4 (TBL) atop Pic du Midi in the French Pyrénées. « Using all three telescopes was essential for monitoring regularly V830 Tau throughout our campaign and for detecting its giant planet » stresses Lison Malo, CFHT astronomer, a coauthor of the study and key to coordinating the observations.

« SPIRou and SPIP, the twin new-generation instruments built for CFHT and TBL by our team and scheduled for first light in 2017 and 2019 respectively, will offer vastly superior performances for such programmes, and will soon allow us to explore the formation of new worlds with unprecedented sensitivity », adds Louise Yu, a coauthor of the study and PhD student in observational exoplanet science at IRAP / OMP.


Contacts

Jean-Francois Donati,IRAP / OMP, Fr, 1st author, t :+33-561332917, e : jean-francois.donati@irap.omp.eu
Claire Moutou, CFHT, Hawaii, 2nd author, t : +1-8088857944, e : moutou@cfht.hawaii.edu
Clément Baruteau, IRAP / OMP, Fr, coauthor, t :+33-561334701, e : clement.baruteau@irap.omp.eu
Louise Yu, IRAP / OMP, Fr, coauthor, e : louise.yu@irap.omp.eu
Elodie Hébrard, York University, Toronto, coauthor, t : +416-736-2100 x44599, e : ehebrard@yorku.ca
Silvia Alencar, UFMG, Brazil, coauthor, t : +55-3134095661, e : silvia@fisica.ufmg.br
Jérome Bouvier, IPAG / OSUG, Fr, coauthor, t : +33-476514790, e : jerome.bouvier@univ-grenoble-alpes.fr
Pascal Petit, IRAP / OMP, Fr, coauthor, t : +33-561332828, e : pascal.petit@irap.omp.eu
Michihiro Takami, ASIAA, Taiwan, coauthor, t : +886-2-2366-5402, e : hiro@asiaa.sinica.edu.tw
Andrew Collier Cameron, Univ of St Andrews, UK, coauthor, t : +44-1334463147, e : acc4@st-andrews.ac.uk

PDF file and complementary images

This press release is also available as a pdf file with complementary illustrations / animations

Additional information

[1] The paper describing the discovery, published in the journal Nature, is available from this link.

[2] IRAP (Institut de Recherche en Astrophysique et Planétologie) is a research lab part of OMP (Observatoire Midi-Pyrénées) located in Toulouse (France), and under dual supervision from CNRS / INSU (Centre National de la Recherche Scientifique / Institut National des Sciences de l’Univers) and UFTMiP / UPS (Université Fédérale Toulouse Midi-Pyrénées / Université Paul Sabatier)

[3] CFHT is operated by the National Research Council of Canada, CNRS/INSU in France and the University of Hawaii.

[4] TBL is operated by IRAP / OMP, CNRS / INSU and UFTMiP / UPS

 

 

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