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Cited by 735Stellar, planetary, and galactic studiesAstronomy and Astrophysical ResearchAstro and Planetary Science

HOT STARS WITH HOT JUPITERS HAVE HIGH OBLIQUITIES

Open access
Winn, Joshua N., Fabrycky, Daniel, Albrecht, Simon, Johnson, John Asher·2010·The Astrophysical Journal
DOI 10.1088/2041-8205/718/2/l145
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Abstract

We show that stars with transiting planets for which the stellar obliquity is large are preferentially hot ( T eff > 6250 K). This could explain why small obliquities were observed in the earliest measurements, which focused on relatively cool stars drawn from Doppler surveys, as opposed to hotter stars that emerged more recently from transit surveys. The observed trend could be due to differences in planet formation and migration around stars of varying mass. Alternatively, we speculate that hot-Jupiter systems begin with a wide range of obliquities, but the photospheres of cool stars realign with the orbits due to tidal dissipation in their convective zones, while hot stars cannot realign because of their thinner convective zones. This in turn would suggest that hot Jupiters originate from few-body gravitational dynamics and that disk migration plays at most a supporting role.

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  • Schlaufman (2010) and Winn et al. (2010) found that among hot Jupiter hosts, only hot stars' spins are misaligned with their hot Jupiters' orbits; cool stars may be more easily tidally realigned.

    “Schlaufman (2010) and Winn et al. (2010) found that among hot Jupiter hosts, only hot stars' spins are misaligned with their hot Jupiters' orbits; cool stars may be more easily tidally realigned (Winn et al. 2010, Albrecht et al. 2012).”

    From Origins of Hot Jupiters (2018) · cites this paper as Winn et al. (2010)

    Split into 2 atoms — 1 confirmed, 1 partially supported, 0 disputed, 0 misattributed, 0 unverifiable. Expand the claim to see per-atom verdicts.

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  • Triaud (2011) reported a trend of host star obliquity decreasing with stellar age, but the trend may instead be with host star effective temperature.

    “For example, Triaud (2011) reported a trend of host star obliquity decreasing with stellar age, but the trend may instead be with host star effective temperature (e.g., Winn et al. 2010).”

    From Origins of Hot Jupiters (2018) · cites this paper as Winn et al. 2010

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Cites

Flagged first, then by citations

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Cited by

Sorted by citations

Authors
Winn, J. N., Fabrycky, D., Albrecht, S., & Johnson, J. A.
Affiliations
  • Massachusetts Institute of Technology (US)
  • Center for Astrophysics Harvard & Smithsonian (US)
  • California Institute of Technology (US)
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2010-07-12
Volume
718
Issue
2
Pages
L145-L149
ISSN
  • 2041-8205 (ISSN-L)
  • 2041-8213
DOI
10.1088/2041-8205/718/2/l145
OpenAlex
W2024502805
Cited by
735
References
1
Citations by year
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FWCI
34.67
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal Letters (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • CaltechAUTHORS (California Institute of Technology) (submittedVersion)
  • DSpace@MIT (Massachusetts Institute of Technology) (submittedVersion, cc-by-nc-sa)
  • arXiv (Cornell University)
Funders
  • National Aeronautics and Space Administration (NNX09AD36G)
  • Nederlandse Organisatie voor Wetenschappelijk Onderzoek
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
Keywords
stellar obliquity, hot Jupiters, hot stars, transiting exoplanets, tidal dissipation, convection zone, planet migration, planet formation, few-body dynamics, disk migration

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