Predictions for a planet just inside Fomalhaut's eccentric ring
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Abstract We propose that the eccentricity and sharpness of the edge of Fomalhaut's disc are due to a planet just interior to the ring edge. The collision time-scale consistent with the disc opacity is long enough that spiral density waves cannot be driven near the planet. The ring edge is likely to be located at the boundary of a chaotic zone in the corotation region of the planet. We find that this zone can open a gap in a particle disc as long as the collision time-scale exceeds the removal or ejection time-scale in the zone. We use the slope measured from the ring edge surface brightness profile to place an upper limit on the planet mass. The removal time-scale in the chaotic zone is used to estimate a lower limit. The ring edge has eccentricity caused by secular perturbations from the planet. These arguments imply that the planet has a mass between that of Neptune and that of Saturn, a semi-major axis of approximately 119 au and longitude of periastron and eccentricity, 0.1, the same as that of the ring edge.
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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).”
Cites
A planetary system as the origin of structure in Fomalhaut's dust belt
Kalas, P., Graham, J. R., & Clampin, M. (2005) · Nature · doi:10.1038/nature03601 · Cited by 411 · see citing works
Models of the dust structures around Vega-excess stars
Dent, W. R. F., Walker, H. J., Holland, W. S., & Greaves, J. S. (2000) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2000.03331.x · Cited by 128 · see citing works
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Optical Images of an Exosolar Planet 25 Light-Years from Earth
Kalas, P., Graham, J. R., Chiang, E., Fitzgerald, M. P., Clampin, M., Kite, E. S., Stapelfeldt, K., Marois, C., & Krist, J. (2008) · Science · doi:10.1126/science.1166609 · Cited by 840 · see citing works
FOMALHAUT'S DEBRIS DISK AND PLANET: CONSTRAINING THE MASS OF FOMALHAUT B FROM DISK MORPHOLOGY
Chiang, E., Kite, E., Kalas, P., Graham, J. R., & Clampin, M. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/693/1/734 · Cited by 223 · see citing works
STIS CORONAGRAPHIC IMAGING OF FOMALHAUT: MAIN BELT STRUCTURE AND THE ORBIT OF FOMALHAUT<i>b</i>
Kalas, P., Graham, J. R., Fitzgerald, M. P., & Clampin, M. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/775/1/56 · Cited by 158 · see citing works
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Mamajek, E. E., Quillen, A. C., Pecaut, M. J., Moolekamp, F., Scott, E. L., Kenworthy, M. A., Cameron, A. C., & Parley, N. R. (2012) · The Astronomical Journal · doi:10.1088/0004-6256/143/3/72 · Cited by 140 · see citing works
“For ξ = 0.2 this gives a planet mass ratio of 2 × 10−5 and for ξ = 0.1 of 2 × 10−4 so planet masses ranging from Saturn to Neptune mass and lower than estimated by Chiang et al. (2009) but consistent with that predicted by Quillen (2006).”
InfluentialSelf-citationTHE SOLAR NEIGHBORHOOD. XXX. FOMALHAUT C
Mamajek, E. E., Bartlett, J. L., Seifahrt, A., Henry, T. J., Dieterich, S. B., Lurie, J. C., Kenworthy, M. A., Jao, W.-C., Riedel, A. R., Subasavage, J. P., et al. (2013) · The Astronomical Journal · doi:10.1088/0004-6256/146/6/154 · Cited by 103 · see citing works
THE GEMINI NICI PLANET-FINDING CAMPAIGN: THE ORBIT OF THE YOUNG EXOPLANET β PICTORIS b
Nielsen, E. L., Liu, M. C., Wahhaj, Z., Biller, B. A., Hayward, T. L., Males, J. R., Close, L. M., Morzinski, K. M., Skemer, A. J., Kuchner, M. J., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/794/2/158 · Cited by 46 · see citing works
- Authors
- Quillen, A. C.
- Affiliations
- University of Rochester (US)
- Corresponding author
- Quillen, Alice C.
- ORCID
- Quillen, Alice C.
- Venue
- Monthly Notices of the Royal Astronomical Society: Letters
- Publisher
- Oxford University Press (OUP)
- Published
- 2006-10-01
- Volume
- 372
- Issue
- 1
- Pages
- L14-L18
- ISSN
- 1745-3925 (ISSN-L)
- 1745-3933
- OpenAlex
- W2126541607
- Cited by
- 167
- References
- 2
- Citations by year
- 2026: 4 · 2025: 2 · 2024: 1 · 2023: 9 · 2022: 1 · 2021: 6 · 2020: 9 · 2019: 1 · 2018: 4 · 2017: 11 · 2016: 10 · 2015: 15 · 2014: 18 · 2013: 15 · 2012: 14
- FWCI
- 5.56
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Monthly Notices of the Royal Astronomical Society Letters (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (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, debris disks, planet-disk interaction, planet mass determination, chaotic zone, secular perturbations, eccentricity, surface brightness profiles, planet mass limits
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