Dynamical modeling of large scale asymmetries in the beta Pictoris dust disk

By Jean Augereau, R. Nelson, Anne-Marie Lagrange, J. Papaloizou, D. D. Grenoble, A. Unit, School of Mathematical Sciences, Queen MaryWestfield College. 2001

165 citations recorded by the source corpus.

We report a new and complete model of the Pictoris disk, which succeeds in accounting for both the surface brightness distribution, warp characteristics, the outer \butterfly" asymmetry as observed by HST/STIS in scattered light, as well as the infrared emission. Our model includes the presence of a disk of planetesimals extending out to 120{150 AU, perturbed gravitationally by a giant planet on an inclined orbit, following the ap- proach of Mouillet et al. (1997b). At any time, the planetesimal disk is assumed to be the source of a distribution of grains produced through collisional evolution, with the same initial orbital parameter distribution. The steady state spatial grain distribution is found incorporating the eects of radiation pressure which can cause the distri- bution of the smallest particles to become very distended. With realistic assumptions about the grains' chemical properties, the modeling conrms the previously evident need for an additional population of hot grains close to the star, to account for the 12m fluxes at short distances from the star. It also indicates that this population cannot explain the outer 12m flux distribution when the eects of gravity and radiation pressure determine the distribution. Very small grains, produced by collisions among aggregates, are tentatively proposed to account for this 12m outer emission.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b15a68cb0cd3de038c20d796250c4e626bdc213c

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In Astronomy and Astrophysics

1. Eric Mamajek
2. M. C. Wyatt
3. S. Kenyon
4. B. Bromley
5. K. Luhman
6. B. Bowler
7. B. Zuckerman
8. Inseok Song

Citations in the corpus

• Collisional processes in extrasolar planetesimal discs – dust clumps in Fomalhaut's debris disc (2002, unknown): “4 of Augereau et al. 2001).”
• The Geometry of Resonant Signatures in Debris Disks with Planets (2002, background): “Disks which are tilted from face-on may show a variety of asymmetries due to effects other than resonant trapping, such as the IRAS/DIRBE dust bands (Hauser et al. 1984), secular warps (Augereau et al. 2001), and limb brightening.”
• Steady State Evolution of Debris Disks around A Stars (2007, background): “…that radiation forces cause the distributions of dust in these systems to extend far beyond those of the planetesimal belts that created them (Augereau et al. 2001), so that the predicted planetesimal belt radii of 24 AU for β Pictoris and 35 AU for HD141569 are not as inaccurate as they…”
• Young Stars Near the Sun (2004, background): “Augereau et al. (2001) model the grain properties and conclude that plantesimals, “parent bodies” for the dust, are located between 20 and 150 AU with a peak at ∼110 AU.”
• A probable giant planet imaged in the beta Pictoris disk. VLT/NaCo deep L'-band imaging (2008, background): “The structure is well reproduced by the deformation induced on colliding planetesimals by a giant planet on a slightly inclined orbit within 50 au from the star (Krist et al. 1996, Mouillet et al. 1997, Gorkavyi et al. 2000, Augereau et al. 2001 and Thébault & Beust 2001).”
• Resonant Trapping of Planetesimals by Planet Migration: Debris Disk Clumps and Vega’s Similarity to the Solar System (2003, background): “…trapped in mean motion resonance with a planet in these systems (Ozernoy et al. 2000; Wyatt & Dent 2002; Quillen & Thorndike 2002; Kuchner & Holman 2003); and a warp in the β Pictoris disk (Heap et al. 2000) may be caused by the perturbations of a planet on an inclined orbit (Augereau et al. 2001).”
• Collisional processes and size distribution in spatially extended debris discs (2007, methodology): “…to the dust’s composition, temperature, optical properties and size distribution, which can never be unambiguously constrained a non–degenerated way (see for instance the thorough best–fit studies of Li & Greenberg (1998) and Augereau et al. (2001) for β Pictoris or Su et al. (2005) for Vega).”
• Collisional Cascades in Planetesimal Disks. II. Embedded Planets (2003, background): “Several disks have asymmetries and warps in their surface brightness distributions (Lagrange et al. 2000; Augereau et al. 2001).”
• A companion to AB Pic at the planet/brown dwarf boundary (2005, background): “In addition, for separations as large as∼ 260 AU, formation by core accretion of planetesimals seems very unlikely because of inappropriate timescales to form planetesimals at such distances (Augereau et al. 2001).”
• PROBING FOR EXOPLANETS HIDING IN DUSTY DEBRIS DISKS: DISK IMAGING, CHARACTERIZATION, AND EXPLORATION WITH HST/STIS MULTI-ROLL CORONAGRAPHY (2014, background): “These are exactly the morphological features predicted to arise in starlight-scattering CS debris perturbed by co-orbiting planets (Wyatt et al. 1999; Augereau et al. 2001; Kuchner & Holman 2003; Wyatt 2003, 2005; Wolf et al. 2007; Ertel et al. 2012).”
• Dust Dynamics, Surface Brightness Profiles, and Thermal Spectra of Debris Disks: The Case of AU Microscopii (2005, background): “The outer disk comprises grains that are only tenuously bound, moving on orbits rendered highly eccentric by stellar wind and radiation forces (e.g., Lecavelier des Etangs et al. 1996; Augereau et al. 2001).”
• Decay of Planetary Debris Disks (2005, background): “As with Vega, the large extent of this system near 10 m requires the presence of very small grains, being ejected by radiation pressure (Augereau et al. 2001).”