Structure in the Dusty Debris around Vega

By D. Wilner, M. Holman, M. Kuchner, Paul T. P. Ho. 2002

147 citations recorded by the source corpus.

We present images of the Vega system obtained with the IRAM Plateau de Bure interferometer at a 1.3 mm wavelength with submillijansky sensitivity and ~2.″5 resolution (about 20 AU). These observations clearly detect the stellar photosphere and two dust emission peaks offset from the star by 9.″5 and 8.″0 to the northeast and southwest, respectively. These offset emission peaks are consistent with the barely resolved structure visible in previous submillimeter images, and they account for a large fraction of the dust emission. The presence of two dust concentrations at the observed locations is plausibly explained by the dynamical influence of an unseen planet of a few Jupiter masses in a highly eccentric orbit that traps dust in principal mean motion resonances.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/26756b1bcbcc79ca51bd8b5cd4666d011ace64ee

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In Astronomy and Astrophysics

1. B. Bowler
2. M. C. Wyatt
3. S. Kenyon
4. B. Bromley
5. K. Luhman
6. T. Löhne
7. A. Krivov
8. C. Marois

In Instrumentation

1. S. Kenyon
2. B. Bowler
3. B. Bromley
4. M. C. Wyatt
5. B. Macintosh
6. C. Marois
7. E. D. Folco
8. R. Doyon

Citations in the corpus

• Collisional processes in extrasolar planetesimal discs – dust clumps in Fomalhaut's debris disc (2002, result): “We note that the resonant ring we propose here is formed in a different manner to that proposed to explain the Vega and ǫ Eridani dust clumps (Ozernoy et al. 2000; Wilner et al. 2002).”
• Steady State Evolution of Debris Disks around A Stars (2007, background): “The inner hole in these belts has been inferred in other studies to be caused by the presence of inner planets (e.g., Roques et al. 1994; Wyatt et al. 1999; Wilner et al. 2002; Wyatt 2003; Quillen 2006).”
• Spitzer IRS Spectroscopy of IRAS-discovered Debris Disks (2006, unknown): “…distances, inferred from SED models, are consistent with the measured radii of HR 4796A, Fomalhaut, and Vega from maps of thermal emission from large particles at mid-infrared and submillimeter wavelengths to within a factor of 2 (Holland et al. 2004; Wilner et al. 2002; Jayawardhana et al. 1998).”
• Imaging Extrasolar Giant Planets (2016, background): “Vega’s nearly face-on debris disk is similar to Fomalhaut’s in terms of its two-component structure comprised of warm and cold dust belts and wide gaps with orbital ratios &10, possibly indicating the presence of multiple low-mass planets (e.g., Wilner et al. 2002; Su et al. 2005; Su et al. 2013).”
• Bright OB stars in the Galaxy. III. Constraints on the radial stratification of the clumping factor (2006, background): “On the other hand, given the fact that Vega has a dust and gas disk (Wilner et al. 2002) which produces an IR excess, one cannot exclude the possibility that a flux calibration based on a comparison of Vega observed magnitudes and model fluxes might lead to systematic errors, at least for λ > 5 µm,…”
• The Geometry of Resonant Signatures in Debris Disks with Planets (2002, background): “Numerical integrations (Wilner et al. 2002) support the idea that these terms to dominate the resonant dynamics over a wide range of planet eccentricities.”
• The Insignificance of P-R drag in detectable extrasolar planetesimal belts (2005, background): “…the inner system which would otherwise be rapidly replenished by P-R drag (e.g., Strom, Edwards & Skrutskie 1993), and clumps arise in models when dust migrates inward due to P-R drag and becomes trapped in a planet’s resonances (Ozernoy et al. 2000; Wilner et al. 2002; Quillen & Thorndike 2002).”
• Resonant Trapping of Planetesimals by Planet Migration: Debris Disk Clumps and Vega’s Similarity to the Solar System (2003, methodology): “…on an eccentric orbit (Wyatt et al. 1999); clumps observed in the ǫ Eridani, Vega and Fomalhaut disks (Holland et al. 1998; Greaves et al. 1998; Wilner et al. 2002; Holland et al. 2003) may be indicative of dust trapped in mean motion resonance with a planet in these systems (Ozernoy et al.…”
• Dust distributions in debris disks: effects of gravity, radiation pressure and collisions (2006, methodology): “…found in most of the debris disks and attributed to the gravity of presumed planets (Wyatt et al. 1999; Ozernoy et al. 2000; Moro-Martín & Malhotra 2002; Quillen & Thorndike 2002; Wyatt & Dent 2002; Wilner et al. 2002; Kuchner & Holman 2003; Moran et al. 2004; Deller & Maddison 2005, among others).”
• The Gemini Deep Planet Survey (2007, background): “In fact, detailed numerical simulations of the effect of giant planets on the dynamical evolution of dusty disks have been able to reproduce the observed morphologies with remarkable agreement (Ozernoy et al. 2000; Wilner et al. 2002; Deller & Maddison 2005).”
• Collisional Cascades in Planetesimal Disks. II. Embedded Planets (2003, background): “The apparent dimensions of the ring, δri ∼ 20 AU at ri ∼ 50 AU and δri ∼ 30 AU at ri ∼ 100 AU, are comparable to the dimensions, δr/r ∼ 0.1–0.2, of the rings in HR 4796A and Vega (Jayawardhana et al. 1998; Koerner et al. 1998; Wilner et al. 2002).”
• Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars (2008, background): “Gas giants rapidly remove debris in the inner disk and impose structure in the debris beyond 30 AU (e.g.,Wilner et al. 2002; Moro-Martı́n &Malhotra 2005).”
• Circumstellar material in the Vega inner system revealed by CHARA/FLUOR (2006, background): “Several studies have shown Vega to harbour a cold circumstellar dust ring ∼85 AU in radius (Holland et al. 1998; Heinrichsen et al. 1998; Koerner et al. 2001; Wilner et al. 2002).”
• Decay of Planetary Debris Disks (2005, background): “Vega also shows a probable circumstellar ring of similar size to that of Fomalhaut in the submillimeter (Wilner et al. 2002).”