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Journal Articles The Astronomical Journal Year : 2018

Dynamical Constraints on the HR 8799 Planets with GPI

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Jason J. Wang
  • Function : Author
James R. Graham
  • Function : Author
Rebekah Dawson
Daniel Fabrycky
Robert J. de Rosa
  • Function : Author
Laurent Pueyo
  • Function : Author
Quinn Konopacky
  • Function : Author
Bruce Macintosh
Christian Marois
Eugene Chiang
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S. Mark Ammons
  • Function : Author
Pauline Arriaga
Vanessa P. Bailey
  • Function : Author
Travis Barman
  • Function : Author
Joanna Bulger
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Jeffrey Chilcote
Tara Cotten
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Rene Doyon
  • Function : Author
Thomas M. Esposito
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Michael P. Fitzgerald
  • Function : Author
Katherine B. Follette
  • Function : Author
Benjamin L. Gerard
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Stephen J. Goodsell
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Alexandra Z. Greenbaum
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Pascale Hibon
  • Function : Author
Li-Wei Hung
  • Function : Author
Patrick Ingraham
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Paul Kalas
James E. Larkin
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Jérôme Maire
  • Function : Author
Franck Marchis
Mark S. Marley
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Stanimir Metchev
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Maxwell A. Millar-Blanchaer
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Eric L. Nielsen
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Rebecca Oppenheimer
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David Palmer
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Jennifer Patience
  • Function : Author
Marshall Perrin
Lisa Poyneer
  • Function : Author
Abhijith Rajan
  • Function : Author
Julien Rameau
  • Function : Author
Fredrik T. Rantakyrö
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Jean-Baptiste Ruffio
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Dmitry Savransky
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Adam C. Schneider
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Anand Sivaramakrishnan
  • Function : Author
Inseok Song
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Remi Soummer
  • Function : Author
Sandrine Thomas
  • Function : Author
J. Kent Wallace
  • Function : Author
Kimberly Ward-Duong
  • Function : Author
Sloane Wiktorowicz
Schuyler Wolff

Abstract

The HR 8799 system uniquely harbors four young super-Jupiters whose orbits can provide insights into the system’s dynamical history and constrain the masses of the planets themselves. Using the Gemini Planet Imager, we obtained down to one milliarcsecond precision on the astrometry of these planets. We assessed four-planet orbit models with different levels of constraints and found that assuming the planets are near 1:2:4:8 period commensurabilities, or are coplanar, does not worsen the fit. We added the prior that the planets must have been stable for the age of the system (40 Myr) by running orbit configurations from our posteriors through N-body simulations and varying the masses of the planets. We found that only assuming the planets are both coplanar and near 1:2:4:8 period commensurabilities produces dynamically stable orbits in large quantities. Our posterior of stable coplanar orbits tightly constrains the planets’ orbits, and we discuss implications for the outermost planet b shaping the debris disk. A four-planet resonance lock is not necessary for stability up to now. However, planet pairs d and e, and c and d, are each likely locked in two-body resonances for stability if their component masses are above 6 M Jup and 7 M Jup, respectively. Combining the dynamical and luminosity constraints on the masses using hot-start evolutionary models and a system age of 42 ± 5 Myr, we found the mass of planet b to be 5.8 ± 0.5 M Jup, and the masses of planets c, d, and e to be {7.2}-0.7+0.6 {M}Jup} each.

Dates and versions

insu-03693525 , version 1 (10-06-2022)

Identifiers

Cite

Jason J. Wang, James R. Graham, Rebekah Dawson, Daniel Fabrycky, Robert J. de Rosa, et al.. Dynamical Constraints on the HR 8799 Planets with GPI. The Astronomical Journal, 2018, 156, ⟨10.3847/1538-3881/aae150⟩. ⟨insu-03693525⟩
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