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Cited by 223Stellar, planetary, and galactic studiesAstro and Planetary ScienceAstrophysics and Star Formation Studies

FOMALHAUT'S DEBRIS DISK AND PLANET: CONSTRAINING THE MASS OF FOMALHAUT B FROM DISK MORPHOLOGY

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Chiang, E., Kite, E., Kalas, P., Graham, J. R., Clampin, M.·2009·The Astrophysical Journal
DOI 10.1088/0004-637x/693/1/734
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Abstract

Following the optical imaging of exoplanet candidate Fomalhaut b (Fom b), we present a numerical model of how Fomalhaut's debris disk is gravitationally shaped by a single interior planet. The model is simple, adaptable to other debris disks, and can be extended to accommodate multiple planets. If Fom b is the dominant perturber of the belt, then to produce the observed disk morphology it must have a mass M pl < 3 M J , an orbital semimajor axis a pl > 101.5 AU, and an orbital eccentricity e pl = 0.11–0.13. These conclusions are independent of Fom b's photometry. To not disrupt the disk, a greater mass for Fom b demands a smaller orbit farther removed from the disk; thus, future astrometric measurement of Fom b's orbit, combined with our model of planet–disk interaction, can be used to determine the mass more precisely. The inner edge of the debris disk at a ≈ 133 AU lies at the periphery of Fom b's chaotic zone, and the mean disk eccentricity of e ≈ 0.11 is secularly forced by the planet, supporting predictions made prior to the discovery of Fom b. However, previous mass constraints based on disk morphology rely on several oversimplifications. We explain why our constraint is more reliable. It is based on a global model of the disk that is not restricted to the planet's chaotic zone boundary. Moreover, we screen disk parent bodies for dynamical stability over the system age of ∼ 100 Myr, and model them separately from their dust grain progeny; the latter's orbits are strongly affected by radiation pressure and their lifetimes are limited to ∼ 0.1 Myr by destructive grain–grain collisions. The single planet model predicts that planet and disk orbits be apsidally aligned. Fomalhaut b's nominal space velocity does not bear this out, but the astrometric uncertainties may be large. If the apsidal misalignment proves real, our calculated upper mass limit of 3 M J still holds. If the orbits are aligned, our model predicts M pl = 0.5 M J , a pl = 115 AU, and e pl = 0.12. Parent bodies are evacuated from mean-motion resonances with Fom b; these empty resonances are akin to the Kirkwood gaps opened by Jupiter. The belt contains at least 3 M ⊕ of solids that are grinding down to dust, their velocity dispersions stirred so strongly by Fom b that collisions are destructive. Such a large mass in solids is consistent with Fom b having formed in situ.

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  • For ξ = 0.2 this gives a planet mass ratio of 2 × 10^-5 and for ξ = 0.1 of 2 × 10^-4, hence ranging from Saturn to Neptune mass and lower than estimated by Chiang et al. (2009) but consistent with that predicted by Quillen (2006).

    “For ξ = 0.2 this gives a planet mass ratio of 2 × 10 -5 and for ξ = 0.1 of 2 × 10 -4 , hence ranging from Saturn to Neptune mass and lower than estimated by Chiang et al. (2009) but consistent with that predicted by Quillen (2006).”

    From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Chiang et al. (2009)

    The Summary (section 4.1; page unavailable) gives Chiang et al.'s conservative constraint as less than 3 Jupiter masses, an upper limit above the Saturn-to-Neptune masses in the citing sentence. It does not estimate a specific mass above that range; the paper also models a 0.1-Jupiter-mass planet (Table 1). Thus the comparison with Chiang's upper limit is supported, but saying the proposed range is lower than Chiang's estimated mass overstates the source. (LLM, conf=0.84)

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Authors
Chiang, E., Kite, E., Kalas, P., Graham, J. R., & Clampin, M.
Affiliations
  • University of California, Berkeley (US)
  • Goddard Space Flight Center (US)
Corresponding author
Chiang, E.
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2009-03-01
Volume
693
Issue
1
Pages
734-749
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/693/1/734
OpenAlex
W2099499874
Semantic Scholar
22b543b547e63f18693bd5f8fda21e528c803a3e
Cited by
223
References
38
Citations by year
2026: 2 · 2025: 3 · 2024: 5 · 2023: 8 · 2022: 7 · 2021: 13 · 2020: 8 · 2019: 6 · 2018: 10 · 2017: 13 · 2016: 15 · 2015: 16 · 2014: 24 · 2013: 25 · 2012: 23
FWCI
11.43
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • arXiv (Cornell University)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
Keywords
Fomalhaut b, planet-disk interaction, disc morphology, gravitational perturbations, mean motion resonance, Kirkwood gaps, chaotic zone, apsidal alignment, grain-grain collisions, radiation pressure, exoplanet candidates

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