Dynamics of the young multiple system GG Tauri

Beust, H.; Dutrey, Anne

doi:10.1051/0004-6361:20053163

Cited by 38 publications

(37 citation statements)

References 28 publications

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“…We found that all stellar flybys with retrograde motions are inefficient leading to very low fractions of stripped planetesimals. This is because they do not move in concert with the passing star and are not gravitationally perturbed for a sufficiently long period of time, as also noted by other authors in similar circumstances (Toomre & Toomre 1972;Beust & Dutrey 2006;Reche et al 2009). All flybys with prograde motion and inclination i ≥ 45 • are also inefficient.…”

Section: Stripping a Debris Disk By Stellar Flybyssupporting

confidence: 58%

Stripping a debris disk by close stellar encounters in an open stellar cluster

Lestrade

Morey

Lassus

et al. 2011

A&A

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A debris disk is a constituent of any planetary system surrounding a main sequence star. We study whether close stellar encounters can disrupt and strip a debris disk of its planetesimals in the expanding open cluster of its birth with a decreasing star number density over 100 Myr. Such stripping would affect the dust production and hence detectability of the disk. We tabulated the fractions of planetesimals stripped off during stellar flybys of miss distances between 100 and 1000 AU and for several mass ratios of the central to passing stars. We then estimated the numbers of close stellar encounters over the lifetime of several expanding open clusters characterized by their initial star densities. We found that a standard disk, with inner and outer radii of 40 and 100 AU, suffers no loss of planetesimals over 100 Myr around a star born in a common embedded cluster with star density ≤1000 pc −3 . In contrast, we found that such a disk is severely depleted of its planetesimals around a star born in an Orion-type cluster where the star density is >20 000 pc −3 . In this environment, a disk loses >97% of its planetesimals around an M-dwarf, >63% around a solar-type star, and >42% around an A-dwarf, over 100 Myr. We roughly estimate that two-thirds of the stars may be born in such high star density clusters. This might explain in part why fewer debris disks are observed around lower mass stars.

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Section: Stripping a Debris Disk By Stellar Flybyssupporting

confidence: 58%

Stripping a debris disk by close stellar encounters in an open stellar cluster

Lestrade

Morey

Lassus

et al. 2011

A&A

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“…Beust & Dutrey 2005, 2006. GG Tau is 1.5 Myr old, but, as noted by Beust & Dutrey (2006), the observed ring may be a transient feature that will undergo significant evolution in the next Myrs. -The data very clearly diffentiate the circumbinary disk from the emission located within the disk: an unresolved source is detected at the position of GG Tau Aa.…”

Section: Discussionmentioning

confidence: 83%

“…These observations place very tight constraints on theoretical model of the dynamical processes leading to the formation of rings in circumbinary systems (e.g. Beust & Dutrey 2005, 2006. GG Tau is 1.5 Myr old, but, as noted by Beust & Dutrey (2006), the observed ring may be a transient feature that will undergo significant evolution in the next Myrs.…”

Section: Discussionmentioning

confidence: 84%

High resolution imaging of the GG Tauri system at 267 GHz

Piétu

Gueth²,

Hily-Blant³

et al. 2011

A&A

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Context. Studying circumbinary disks is critical to understanding the formation mechanisms of binary stars. While optical or midinfrared images reveal the scattered emission, millimeter observations provide direct measurements of the dust thermal emission. Aims. We study the properties of the circumbinary disk around the well-known, multiple young stellar object GG Tau with the highest possible sensitivity and spatial resolution. Methods. We mapped the continuum emission of GG Tau at 267 GHz using the IRAM Plateau de Bure interferometer equipped with upgraded receivers and LO systems. An angular resolution of 0.45 × 0.25 was achieved, corresponding to a linear resolution of 65 × 35 AU. Results. The GG Tau A circumbinary disk is observed as an extremely clearly defined narrow ring. The width of the ring is not resolved. Emission from the central binary is detected and clearly separated from the ring: it coincides with the GG Tau Aa position and may therefore trace a circumstellar disk around this star. The mass ratio of the circumbinary to circumprimary material is ∼80.

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“…This permits us to perform an analysis without any restriction on the eccentricities. The resulting Hamiltonian is given by Krymolowski & Mazeh (1999), Ford et al (2000), or Beust & Dutrey (2006).…”

Section: Analytical Approachmentioning

confidence: 99%

Can eccentric debris disks be long-lived?

Faramaz

Beust

Thébault

et al. 2014

A&A

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Context. Imaging of debris disks has found evidence for both eccentric and offset disks. One hypothesis is that they provide evidence for massive perturbers, for example, planets or binary companions, which sculpt the observed structures. One such disk was recently observed in the far-IR by the Herschel Space Observatory around ζ 2 Reticuli. In contrast with previously reported systems, the disk is significantly eccentric, and the system is several Gyr old. Aims. We aim to investigate the long-term evolution of eccentric structures in debris disks caused by a perturber on an eccentric orbit around the star. We hypothesise that the observed eccentric disk around ζ 2 Reticuli might be evidence of such a scenario. If so, we are able to constrain the mass and orbit of a potential perturber, either a giant planet or a binary companion. Methods. Analytical techniques were used to predict the effects of a perturber on a debris disk. Numerical N-body simulations were used to verify these results and further investigate the observable structures that may be produced by eccentric perturbers. The longterm evolution of the disk geometry was examined, with particular application to the ζ 2 Reticuli system. In addition, synthetic images of the disk were produced for direct comparison with Herschel observations. Results. We show that an eccentric companion can produce both the observed offsets and eccentric disks. These effects are not immediate, and we characterise the timescale required for the disk to develop to an eccentric state (and any spirals to vanish). For ζ 2 Reticuli, we derive limits on the mass and orbit of the companion required to produce the observations. Synthetic images show that the pattern observed around ζ 2 Reticuli can be produced by an eccentric disk seen close to edge-on, and allow us to bring additional constraints on the disk parameters of our model (disk flux and extent). Conclusions. We conclude that eccentric planets or stellar companions can induce long-lived eccentric structures in debris disks. Observations of such eccentric structures thus provide potential evidence of the presence of such a companion in a planetary system. We considered the specific example of ζ 2 Reticuli, whose observed eccentric disk can be explained by a distant companion (at tens of AU) on an eccentric orbit (e p 0.3).

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Dynamics of the young multiple system GG Tauri

Cited by 38 publications

References 28 publications

Stripping a debris disk by close stellar encounters in an open stellar cluster

Stripping a debris disk by close stellar encounters in an open stellar cluster

High resolution imaging of the GG Tauri system at 267 GHz

Can eccentric debris disks be long-lived?

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