Signatures of the Giant Planets Imprinted on the Edgeworth-Kuiper Belt Dust Disk

Liou, J.‐C.; Zook, H. A.

doi:10.1086/300938

Cited by 180 publications

(209 citation statements)

References 32 publications

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“…The combination of resolved disk maps and planet imaging is an especially powerful tool to understand the planet-disk interactions that may sculpt young planetary systems (e.g. Liou & Zook 1999;Kuchner & Holman 2003;Wyatt 2006;Quillen & Faber 2006). The structure of the Fomalhaut disk inner edge has been compared with dynamical models of planets with different masses (Chiang et al 2009), and the size and shape of the HR 8799 disk have been compared with models of the dynamically cleared zones and orbital migration history (Patience et al 2011).…”

Section: Discussionmentioning

confidence: 99%

The International Deep Planet Survey

Vigan

Patience

Marois

et al. 2012

A&A

155

200

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Breakthrough direct detections of planetary companions orbiting A-type stars confirm the existence of massive planets at relatively large separations, but dedicated surveys are required to estimate the frequency of similar planetary systems. To measure the first estimation of the giant exoplanetary systems frequency at large orbital separation around A-stars, we have conducted a deep-imaging survey of young (8−400 Myr), nearby (19−84 pc) A-and F-stars to search for substellar companions in the ∼10−300 AU range. The sample of 42 stars combines all A-stars observed in previous AO planet search surveys reported in the literature with new AO observations from VLT/NaCo and Gemini/NIRI. It represents an initial subset of the International Deep Planet Survey (IDPS) sample of stars covering M-to B-stars. The data were obtained with diffraction-limited observations in H-and K s -band combined with angular differential imaging to suppress the speckle noise of the central stars, resulting in typical 5σ detection limits in magnitude difference of 12 mag at 1 , 14 mag at 2 and 16 mag at 5 which is sufficient to detect massive planets. A detailed statistical analysis of the survey results is performed using Monte Carlo simulations. Considering the planet detections, we estimate the fraction of A-stars having at least one massive planet (3−14 M Jup ) in the range 5−320 AU to be inside 5.9−18.8% at 68% confidence, assuming a flat distribution for the mass of the planets. By comparison, the brown dwarf (15−75 M Jup ) frequency for the sample is 2.0−8.9% at 68% confidence in the range 5−320 AU. Assuming power law distributions for the mass and semimajor axis of the planet population, the AO data are consistent with a declining number of massive planets with increasing orbital radius which is distinct from the rising slope inferred from radial velocity (RV) surveys around evolved A-stars and suggests that the peak of the massive planet population around A-stars may occur at separations between the ranges probed by existing RV and AO observations. Finally, we report the discovery of three new close M-star companions to HIP 104365 and HIP 42334.

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Section: Discussionmentioning

confidence: 99%

The International Deep Planet Survey

Vigan

Patience

Marois

et al. 2012

A&A

155

200

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“…The (3 Pic disk has several subtle asymmetries such as differences in its radial brightness profile and vertical thickness between the NE and SW extensions (22); one possible explanation is that the disk was recently disturbed by the close passage of an as-yet-unidentified M dwarf star. The e Eri dust ring appears to have major azimuthal clumps and voids which can plausibly be forced by a jovian planet orbiting near or within the ring (27). Finally, a most unusual variable brightness asymmetry has been observed in optical images of HH 30: a bright spot of light appears to be moving around the disk (45).…”

Section: Stapelfeldtmentioning

confidence: 99%

Visions of Nature's Planet Foundry: Images of Circumstellar Disks

Stapelfeldt

2004

Symp. - Int. Astron. Union

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Abstract.As the number of detected extrasolar planetary systems has steadily grown over the past five years, so too has the number of circumstellar disks with resolved images. In this contribution, I take stock of the current inventory of disk images at various wavelengths; summarize the results of a new disk imaging survey conducted with the Hubble Space Telescope; review the major inferences that can be drawn about disk structure from the extant images; and suggest areas for future progress.

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“…Spectroscopic observations from 5.3-40 µm enable diagnosis of gaps caused by giant planets [9] and estimates of dust size and composition which translate directly into constraints on the mass opacity coeffients for the dust [14] as well as Poynting-Robertson drag timescales [1]. Fig.…”

Section: Mature Solar System Evolutionmentioning

confidence: 99%

The Formation and Evolution of Planetary Systems: SIRTF Legacy Science in the VLT Era

Meyer

Backman

Beckwith³

et al. 2002

The Origins of Stars and Planets: The VLT View

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Abstract. We will utilize the sensitivity of SIRTF through the Legacy Science Program to carry out spectrophotometric observations of solar-type stars aimed at (1) defining the timescales over which terrestrial and gas giant planets are built, from measurements diagnostic of dust/gas masses and radial distributions; and (2) establishing the diversity of planetary architectures and the frequency of planetesimal collisions as a function of time through observations of circumstellar debris disks. Together, these observations will provide an astronomical context for understanding whether our solar system -and its habitable planet -is a common or a rare circumstance.Achieving our science goals requires measuring precise spectral energy distributions for a statistically robust sample capable of revealing evolutionary trends and the diversity of system outcomes. Our targets have been selected from two carefully assembled databases of solar-like stars: (1) a sample located within 50 pc of the Sun spanning an age range from 100-3000 Myr for which a rich set of ancillary measurements (e.g. metallicity, stellar activity, kinematics) are available; and (2) a selection located between 15 and 180 pc and spanning ages from 3 to 100 Myr. For stars at these distances SIRTF is capable of detecting stellar photospheres with SNR >30 at λ ≤ 24µm for our entire sample, as well as achieving SNR >5 at the photospheric limit for over 50% of our sample at λ = 70µm. Thus we will provide a complete census of stars with excess emission down to the level produced by the dust in our present-day solar system. SIRTF observations obtained as part of this program will provide a rich Legacy for follow-up observations utilizing a variety of facilities including the VLT. More information concerning our program can be found at http://gould.as.arizona.edu/feps.

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Signatures of the Giant Planets Imprinted on the Edgeworth-Kuiper Belt Dust Disk

Cited by 180 publications

References 32 publications

The International Deep Planet Survey

The International Deep Planet Survey

Visions of Nature's Planet Foundry: Images of Circumstellar Disks

The Formation and Evolution of Planetary Systems: SIRTF Legacy Science in the VLT Era

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