The Geometry of Resonant Signatures in Debris Disks with Planets

By M. Kuchner, M. Holman. 2002

135 citations recorded by the source corpus.

Using simple geometrical arguments, we paint an overview of the variety of resonant structures a single planet with moderate eccentricity (e ≲ 0.6) can create in a dynamically cold, optically thin dust disk. This overview may serve as a key for interpreting images of perturbed debris disks and inferring the dynamical properties of the planets responsible for the perturbations. We compare the resonant geometries found in the solar system dust cloud with observations of dust clouds around Vega, ϵ Eridani, and Fomalhaut.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/312f729796ffbfc65625239a429365ac9d8ec1d1

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In Astronomy and Astrophysics

1. S. Kenyon
2. B. Bromley
3. M. C. Wyatt
4. R. Malhotra
5. T. Löhne
6. A. Krivov
7. Thomas H. Jarrett
8. M. Sremčević

Citations in the corpus

• Dust distributions in debris disks: effects of gravity, radiation pressure and collisions (2006, background): “…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).”
• NEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THE SPITZER SPACE TELESCOPE (2009, unknown): “In Equations A28 and A29, Dp+q:q corresponds to the semi-major axis of the orbital resonance p+q:p, which can be related to the planet semi-major axis as in Krivov et al. (2007): Dp+q:q = Dpl (1 − β) 1/3 ( p + q p )2/3 (A31) From Equation A29 we conclude that a proto-planet >0.05MJ at 50 AU will tra”
• 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).”
• The Size Distribution of Trans-Neptunian Bodies (2003, background): “Some of these dust disks exhibit structures that can perhaps be ascribed to embedded planetary systems (Kuchner & Holman 2003).”
• THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE): MISSION DESCRIPTION AND INITIAL ON-ORBIT PERFORMANCE (2010, background): “The disk does not clear uniformly due to both the variation in accretion/dynamical timescale with distance from the star, and the shepherding effects of forming planets (Kuchner & Holman 2003).”
• Resonant Trapping of Planetesimals by Planet Migration: Debris Disk Clumps and Vega’s Similarity to the Solar System (2003, background): “…of dust 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…”
• The Insignificance of P-R drag in detectable extrasolar planetesimal belts (2005, background): “This also means that azimuthal structure in the disks cannot be caused by dust migrating into the resonances of a planet (e.g., Kuchner & Holman 2003), at least not due to P-R drag alone.”
• Collisional Cascades in Planetesimal Disks. II. Embedded Planets (2003, background): “Resonant interactions between dust and distant large planets (Wilner et al. 2002; Kuchner & Holman 2003) or small moons (Wyatt et al. 1999) can produce rings or ring arcs in the disk.”