Dynamical modeling of large scale asymmetries in the <i>β</i> Picto ris dust disk

Augereau, J.-C.; Nelson, Richard P.; Lagrange, A. M.; Papaloizou, J. C. B.; Mouillet, D.

doi:10.1051/0004-6361:20010199

Cited by 303 publications

(524 citation statements)

References 17 publications

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“…Recent results by Chauvin et al (2012), including measurements from this survey, refined the orbital parameters with a semi-major axis of 8−9 AU and an eccentricity lower than e ≤ 0.17. In addition, Lagrange et al (2012a) could accurately show that the planet is located in the second-warped component of the debris disk surrounding the star, which confirms previous studies (Mouillet et al 1997;Augereau et al 2001) that suggested that the planet plays a key role in the morphology of the disk. More recently, Lagrange et al (2012b) directly constrained the mass of the planet through eight years of high-precision RV data, offering thus a rare perspective for the calibration of mass-luminosity relation of young massive Fig.…”

Section: Substellar Companionssupporting

confidence: 85%

“…Observations at several wavelengths revealed asymmetry structures, sometimes ringlike, or even warps, which could arise from gravitational perturbations imposed by one or more giant planets (e.g. Mouillet et al 1997;Augereau et al 2001;Kalas et al 2005). Thanks to the improvement of direct imaging (DI) technique with groundbased adaptive optics systems (AO) or space telescopes, a few planetary mass objects and low-mass brown dwarfs have been detected since the first detection by Chauvin et al (2004).…”

Section: Introductionmentioning

confidence: 99%

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A survey of young, nearby, and dusty stars conducted to understand the formation of wide-orbit giant planets

Rameau

Chauvin

Lagrange

et al. 2013

A&A

107

148

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Context. Over the past decade, direct imaging has confirmed the existence of substellar companions on wide orbits from their parent stars. To understand the formation and evolution mechanisms of these companions, their individual as well as the full population properties must be characterized. Aims. We aim at detecting giant planet and/or brown dwarf companions around young, nearby, and dusty stars. Our goal is also to provide statistics on the population of giant planets at wide-orbits and discuss planet formation models. Methods. We report the results of a deep survey of 59 stars, members of young stellar associations. The observations were conducted with the ground-based adaptive optics system VLT/NaCo at L -band (3.8 μm). We used angular differential imaging to reach the best detection performances down to the planetary mass regime. A statistical analysis of about 60% of the young and southern A-F stars closer than 65 pc allowed us to derive the fraction of giant planets on wide orbits. We used gravitational instability models and planet population synthesis models following the core-accretion scenario to discuss the occurrence of these companions. Results. We resolve and characterize new visual binaries and do not detect any new substellar companion. The survey's median detection performance reaches contrasts of 10 mag at 0.5 and 11.5 mag at 1.0 . We find the occurrence of planets to be between 10.8 and 24.8% at 68% confidence level assuming a uniform distribution of planets in the interval [1, 13] M J and [1, 1000] AU. Considering the predictions of planetary formation models, we set important constraints on the occurrence of massive planets and brown dwarf companions that would have formed by gravitational instability. We show that this mechanism favors the formation of rather massive clumps (M clump > 30 M J ) at wide (a > 40 AU) orbits, which may evolve dynamically and/or fragment. For the population of close-in giant planets that would have formed by core accretion (without considering any planet -planet scattering), our survey marginally explores physical separations (≤20 AU) and cannot constrain this population. We will have to wait for the next generation of planet finders to start exploring that population, and even for the extremely large telescopes for a more complete overlap with other planet-hunting techniques.

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Section: Substellar Companionssupporting

confidence: 85%

Section: Introductionmentioning

confidence: 99%

A survey of young, nearby, and dusty stars conducted to understand the formation of wide-orbit giant planets

Rameau

Chauvin

Lagrange

et al. 2013

A&A

107

148

View full text Add to dashboard Cite

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“…Weissman 1995). However, this is also a region which, according to most models, is dust depleted (with a peak at ∼100−120 AU and a relative inner hole inside 50 AU; Augereau et al 2001). This is an interesting paradox, which goes beyond the scope of the present paper, but would have to be explained within the frame of a global coherent model of the β Pic system.…”

Section: β Pictorismentioning

confidence: 75%

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

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Context. Previous observations with the Infrared Astronomical Satellite and the Infrared Space Observatory, and ongoing observations with Spitzer and AKARI, have led to the discovery of over 200 debris disks, based on detected mid-and far infrared excess emission, indicating warm circumstellar dust. To constrain the properties of these systems, e.g., to more accurately determine the dust mass, temperature and radial extent, follow-up observations in the submillimetre wavelength region are needed. Aims. The β Pictoris moving group is a nearby stellar association of young (∼12 Myr) co-moving stars including the classical debris disk star β Pictoris. Due to their proximity and youth, they are excellent targets when searching for submillimetre emission from cold, extended, dust components produced by collisions in Kuiper-Belt-like disks. They also allow an age independent study of debris disk properties as a function of other stellar parameters. Methods. We observed 7 infrared-excess stars in the β Pictoris moving group with the LABOCA bolometer array, operating at a central wavelength of 870 μm at the 12-m submillimetre telescope APEX. The main emission at these wavelengths comes from large, cold dust grains, which constitute the main part of the total dust mass, and hence, for an optically thin case, make better estimates on the total dust mass than earlier infrared observations. Fitting the spectral energy distribution with combined optical and infrared photometry gives information on the temperature and radial extent of the disk. Results. From our sample, β Pic, HD 181327, and HD 172555 were detected with at least 3σ certainty, while all others are below 2σ and considered non-detections. The image of β Pic shows an offset flux density peak located near the south-west extension of the disk, similar to the one previously found by SCUBA at the JCMT. We present SED fits for detected sources and give an upper limit on the dust mass for undetected ones. Conclusions. We find a mean fractional dust luminosityf dust = 1.1 × 10 −3 at t ≈ 12 Myr, which together with recent data at 100 Myr suggests an f dust ∝ t −α decline of the emitting dust, with α > 0.8.

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“…We model the subsequent evolution of this gaseous component using standard accretion disc physics. The modelled gas sits in a dust disc, which extends from ∼ 50 to ∼ 150AU (Augereau et al 2001;Dent et al 2014) and might affect the thermal state of the gas. Throughout this paper, we choose to use our general model on β Pic so that we take the gas injection location to be R0 = 85 AU, where the bulk of CO is located.…”

Section: Numerical Model For Gas Evolutionmentioning

confidence: 99%

A self-consistent model for the evolution of the gas produced in the debris disc of β Pictoris

Kral¹,

Wyatt²,

Carswell³

et al. 2016

Mon. Not. R. Astron. Soc.

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This paper presents a self-consistent model for the evolution of gas produced in the debris disc of β Pictoris. Our model proposes that atomic carbon and oxygen are created from the photodissociation of CO, which is itself released from volatile-rich bodies in the debris disc due to grain-grain collisions or photodesorption. While the CO lasts less than one orbit, the atomic gas evolves by viscous spreading resulting in an accretion disc inside the parent belt and a decretion disc outside. The temperature, ionisation fraction and population levels of carbon and oxygen are followed with the photodissociation region model Cloudy, which is coupled to a dynamical viscous α model. We present new gas observations of β Pic, of C I observed with APEX and O I observed with Herschel, and show that these along with published C II and CO observations can all be explained with this new model. Our model requires a viscosity α > 0.1, similar to that found in sufficiently ionised discs of other astronomical objects; we propose that the magnetorotational instability is at play in this highly ionised and dilute medium. This new model can be tested from its predictions for high resolution ALMA observations of C I. We also constrain the water content of the planetesimals in β Pic. The scenario proposed here might be at play in all debris discs and this model could be used more generally on all discs with C, O or CO detections.

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Dynamical modeling of large scale asymmetries in the β Picto ris dust disk

Cited by 303 publications

References 17 publications

A survey of young, nearby, and dusty stars conducted to understand the formation of wide-orbit giant planets

A survey of young, nearby, and dusty stars conducted to understand the formation of wide-orbit giant planets

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

A self-consistent model for the evolution of the gas produced in the debris disc of β Pictoris

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