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Cited by 158Stellar, planetary, and galactic studiesAstro and Planetary ScienceGalaxies: Formation, Evolution, Phenomena

FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION

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Ngo, Henry, Knutson, Heather A., Hinkley, Sasha, Bryan, Marta, Crepp, Justin R., Batygin, Konstantin, Crossfield, Ian, Hansen, Brad +6 more·2016·The Astrophysical Journal
DOI 10.3847/0004-637x/827/1/8
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Abstract

Stellar companions can influence the formation and evolution of planetary systems, but there are currently few observational constraints on the properties of planet-hosting binary star systems. We search for stellar companions around 77 transiting hot Jupiter systems to explore the statistical properties of this population of companions as compared to field stars of similar spectral type. After correcting for survey incompleteness, we find that of hot Jupiter systems have stellar companions with semimajor axes between 50 and 2000 au. This is 2.9 times larger than the field star companion fraction in this separation range, with a significance of . In the 1–50 au range, only of hot Jupiters host stellar companions, compared to the field star value of , which is a difference. We find that the distribution of mass ratios for stellar companions to hot Jupiter systems peaks at small values and therefore differs from that of field star binaries which tend to be uniformly distributed across all mass ratios. We conclude that either wide separation stellar binaries are more favorable sites for gas giant planet formation at all separations, or that the presence of stellar companions preferentially causes the inward migration of gas giant planets that formed farther out in the disk via dynamical processes such as Kozai–Lidov oscillations. We determine that less than 20% of hot Jupiters have stellar companions capable of inducing Kozai–Lidov oscillations assuming initial semimajor axes between 1 and 5 au, implying that the enhanced companion occurrence is likely correlated with environments where gas giants can form efficiently.

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  • Most companions to hot Jupiters are not massive and nearby enough to overcome general relativistic and tidal precession.

    “Most companions are not massive and nearby enough to overcome general relavistic (Eqn. 14) and tidal precession.”

    From Origins of Hot Jupiters (2018) · cites this paper as Ngo et al. (2016)

    Section 6.2 evaluates whether stellar companions are massive and close enough to induce Kozai–Lidov oscillations despite general-relativistic pericenter precession; the Abstract reports that fewer than 20% of hot Jupiters have capable companions under the stated initial-orbit assumptions. The paper does not include tidal precession in that calculation, so it does not support that part of the claim. Page numbers were not provided in our copy. (LLM, conf=0.86)

    Experimental — accuracy not yet measured

  • The properties of hot Jupiters' stellar companions are incompatible with high eccentricity migration triggered by stellar Kozai being the dominant channel of formation.

    “The properties of hot Jupiters' stellar companions are incompatible with high eccentricity migration triggered by stellar Kozai being the dominant channel of formation.”

    From Origins of Hot Jupiters (2018) · cites this paper as Ngo et al. (2016)

    Section 6.2 finds that the observed companions are often too low-mass and widely separated to drive the required migration, and concludes that Kozai–Lidov oscillations cannot be the dominant mechanism for transiting hot Jupiters found by ground-based surveys. The claim extends that conclusion to hot Jupiters generally, whereas the paper cautions that survey selection biases may make its sample unrepresentative of the entire population. Page numbers are unavailable in our copy. (LLM, conf=0.82)

    Experimental — accuracy not yet measured

  • Ngo et al. (2016) found an upper limit of 16 ± 5% on hot Jupiters with stellar companions capable of triggering high eccentricity tidal migration via Kozai-Lidov cycles if the hot Jupiter formed between ∼1-5 AU.

    “Ngo et al. (2016) found an upper limit of 16 ± 5% on hot Jupiters with stellar companions capable of triggering high eccentricity tidal migration via Kozai-Lidov cycles (if the hot Jupiter formed between ∼ 1-5 AU).”

    From Origins of Hot Jupiters (2018) · cites this paper as Ngo et al. (2016)

  • Ngo et al. (2016) find no correlation between binary companions and spin-orbit misalignments.

    “Ngo et al. (2016) find no correlation between binary companions and spin-orbit misalignments.”

    From Origins of Hot Jupiters (2018) · cites this paper as Ngo et al. (2016)

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Authors
Ngo, H., Knutson, H. A., Hinkley, S., Bryan, M., Crepp, J. R., Batygin, K., Crossfield, I., Hansen, B., Howard, A. W., Johnson, J. A., Mawet, D., Morton, T. D., Muirhead, P. S., & Wang, J.
Affiliations
  • California Institute of Technology (US)
  • University of Exeter (GB)
  • University of Notre Dame (US)
  • University of Arizona (US)
  • University of California, Los Angeles (US)
  • University of Hawaiʻi at Mānoa (US)
  • Smithsonian Astrophysical Observatory (US)
  • Princeton University (US)
  • Boston University (US)
Corresponding author
Ngo, Henry
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2016-08-03
Volume
827
Issue
1
Pages
8
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.3847/0004-637x/827/1/8
OpenAlex
W2465266626
Cited by
158
References
0
Citations by year
2026: 9 · 2025: 21 · 2024: 13 · 2023: 13 · 2022: 16 · 2021: 15 · 2020: 20 · 2019: 9 · 2018: 17 · 2017: 20 · 2016: 5
FWCI
8.13
Type
journal article
Language
en
Open access
Licence
Locations
  • The Astrophysical Journal (publishedVersion)
  • UA Campus Repository (The University of Arizona) (acceptedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • CaltechAUTHORS (California Institute of Technology) (submittedVersion)
  • OpenBU (Boston University) (submittedVersion)
  • arXiv (Cornell University)
Funders
  • National Aeronautics and Space Administration (NNX14AD24G, NNX15AR12H)
  • California Institute of Technology
  • Natural Sciences and Engineering Research Council of Canada
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 › Galaxies: Formation, Evolution, Phenomena
Keywords
hot Jupiters, stellar companions, binary stars, Kozai-Lidov oscillations, planet migration, gas giant planet formation, transiting exoplanets, wide binaries, field stars

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