HOT STARS WITH HOT JUPITERS HAVE HIGH OBLIQUITIES

By J. Winn, D. Fabrycky, S. Albrecht, J. Johnson. 2010

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We show that stars with transiting planets for which the stellar obliquity is large are preferentially hot (Teff > 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.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ecec76d69db9f8db8059b9f4039b5e7d4e54a1a6

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Citations in the corpus

Tidal dissipation in planet-hosting stars: damping of spin-orbit misalignment and survival of hot Jupiters (2011, background): “Indeed, the facts that effective temperature is more closely related to obliquity than stellar mass and that a few low-mass and longperiod planets are exceptions to the Θ − Teff correlation (Winn et al. 2010,2011), support the idea of tidal damping of spin-orbit misalignment in solar-type stars.”
THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, background): “The subsequent discovery of highly inclined or even retrograde hot Jupiters has therefore again challenged theory (e.g., Winn et al. 2010).”
THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS (2016, background): “…2006; Kratter & Perets 2012; Kaib et al. 2013), though dynamical interactions also have been suggested as a channel for producing the many giant planets discovered well inside the snow line (Kozai 1962; Fabrycky & Tremaine 2007; Winn et al. 2010; Naoz et al. 2012; but also Ngo et al. 2015).”
A STUDY OF THE SHORTEST-PERIOD PLANETS FOUND WITH KEPLER (2014, background): “…of the host stars to see if their rotation axes are frequently misaligned with the planetary orbits, as is the case with hot Jupiters (see, e.g., Winn et al. 2010; Triaud et al. 2010; Albrecht et al. 2012), or whether they have low obliquities similar to many of the multi-transit host…”
Asteroseismology of Solar-Type and Red-Giant Stars (2013, positive): “Theories which propose that strong misalignments are the result of dynamical interactions (e.g., see Winn et al. 2010) are supported by the well-ordered alignments found in the multi-planet system Kepler-30 studied by Sanchis-Ojeda et al. (2012) using spot-crossing data; and two multiple-systems…”
TIDAL EVOLUTION OF CLOSE-IN PLANETS (2010, background): “Recently, Winn et al. (2010a) suggested that the stellar obliquity is preferentially large for hot stars with effective temperatures Teff > 6250K, and proposed that such a trend can be explained because photospheres of cool stars can realign with the orbits due to tidal dissipation in the…”
SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, background): “KeplerGiants_arXiv even more questions and complexity in the planet formation and evolution (Winn et al. 2010; Hébrard et al. 2010; Triaud 2011; Dawson 2014).”
SECULAR CHAOS AND THE PRODUCTION OF HOT JUPITERS (2010, background): “The current situation is best summarized in Morton & Johnson (2011), and a correlation between stellar obliquity and stellar spectral type has been noted (Winn et al. 2010).”
TOWARD CHEMICAL CONSTRAINTS ON HOT JUPITER MIGRATION (2014, background): “…number of large spin-orbit misalignments observed in hot Jupiter systems initially supported the rol of migration by scattering phenomena (e.g. Winn et al. 2010), but such misalignments may also be caused by planet migration through disks that are themselves misaligned (Batygin 2012; Crida &…”
PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “…that span the range e = 0–0.93 (e.g., Marcy et al. 2005b; Udry & Santos 2007; Moorhead et al. 2011), and the close-in “hot Jupiters” show a wide distribution of inclinations relative to the equatorial plane of the host star (Winn et al. 2010, 2011; Triaud et al. 2010; Morton & Johnson 2011a).”
THE STATISTICS OF MULTI-PLANET SYSTEMS (2011, background): “…oscillations, planet–planet scattering, and resonance sweeping; (4) measurements of the Rossiter–McLaughlin effect in transiting systems (e.g., Winn et al. 2010) show a broad distribution of obliquities (angle between the spin axis of the host star and the orbit axis of the planet) and…”
Tidal Dissipation in Stars and Giant Planets (2014, background): “Winn et al. (2010) argued that most of the cooler stars (Teff < 6250K) are aligned, while the hotter stars have widely spread obliquities.”
The Eccentric Kozai-Lidov Effect and Its Applications (2016, background): “the prediction of retrograde Hot Jupiters (i.e., obliquities larger than 90) (Fabrycky and Tremaine 2007; Wu et al. 2007). The recent detections of retrograde Hot Jupiters (e.g., Triaud et al. 2010; Winn et al. 2010; Albrecht et al. 2012b) resulted in a new interest in the possibility that secular t”
WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, result): “This result could favor Q′?,0 values & 10 7 for WASP-121, which would be in line with the expectation that hot stars (Teff > 6250 K) would have low tidal dissipation efficiencies due to their thin or quasi-nonexistent convective envelopes (see e.g. Winn et al. 2010, Albrecht et al. 2012).”
Tidal obliquity evolution of potentially habitable planets (2011, background): “…points towards a more complex formation scenario, where the stellar obliquity, i.e. the misalignment between thest llar rotation axis and the orbital plane normal, depends on stellar and planetary mass (Winn et al. 2010) as well as on the influence of perturbing bodies (Fabrycky & Tremaine 2007).”