Misaligned spin-orbit in the XO-3 planetary system?†

By G. Hébrard, F. Bouchy, F. Pont, B. Loeillet, M. Rabus, X. Bonfils, C. Moutou, I. Boisse, X. Delfosse, M. Desort and 13 more. Proceedings of the International Astronomical Union, 2008

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Abstract The SOPHIE Consortium started a large program of exoplanets search and characterization in the Northern hemisphere with the new spectrograph SOPHIE at the 1.93-m telescope of Haute-Provence Observatory, France. The objectives of this program are to characterize the zoo of exoplanets and to bring strong constraints on their processes of formation and evolution using the radial velocity technique. We present here new SOPHIE measurements of the transiting planet host star XO-3. This allowed us to observe the Rossiter-McLaughlin effect and to refine the parameters of the planet. The unusual shape of the radial velocity anomaly during the transit provides a hint for a nearly transverse Rossiter-McLaughlin effect. The sky-projected angle between the planetary orbital axis and the stellar rotation axis should be λ = 70° ± 15° to be compatible with our observations. This suggests that some close-in planets might result from gravitational interaction between planets and/or stars rather than migration. This result requires confirmation by additional observations.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

OBLIQUITIES OF HOT JUPITER HOST STARS: EVIDENCE FOR TIDAL INTERACTIONS AND PRIMORDIAL MISALIGNMENTS (2012, background): “Since then many systems have been studied, including those with misaligned stars (Hébrard et al. 2008), retrograde orbits (Winn et al. 2009; Triaud et al. 2010), a hot Neptune (Winn et al. 2010c; Hirano et al. 2011b) and even a circumbinary planet (Winn et al. 2011b).”
Tidal dissipation in planet-hosting stars: damping of spin-orbit misalignment and survival of hot Jupiters (2011, background): “…shown that a significant fraction of hot Jupiter systems have misaligned stellar spin with respect to the planetary angular momentum axis (e.g., Hébrard et al. 2008; Winn et al. 2009,2010,2011; Johnson et al. 2009; Narita et al. 2009; Triaud et al. 2010; Pont et al. 2010; Simpson et al. 2011;…”
HOT STARS WITH HOT JUPITERS HAVE HIGH OBLIQUITIES (2010, background): “Then in a sudden reversal, several misaligned systems were found, with the first sighting by Hébrard et al. (2008) and the most recent spate of discoveries by Triaud et al. (2010).”
PHYSICS OF ECLIPSING BINARIES. II. TOWARD THE INCREASED MODEL FIDELITY (2016, background): “The misalignment has also been found for a number of “hot Jupiters” (Hébrard et al. 2008).”
Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, background): “XO-3 is also known to exhibit a large spin-orbit misalignment (Hébrard et al. 2008; Winn et al. 2009) suggestive of dynamic l evolution through gravitational interactions (e.g. Fabrycky & Winn 2009).”
The Occurrence and Architecture of Exoplanetary Systems (2014, background): “Measurements of stellar obliquity have revealed a wide range of configurations, including stars with lower obliquities than the Sun (e.g., HD 189733; Winn et al. 2006), stars with moderate tilts (e.g., XO-3; Hébrard et al. 2008, Winn et al. 2009, Hirano et al. 2011), stars that are apparently spinn”
The Rossiter-McLaughlin effect of CoRoT-3b and HD 189733b (2009, background): “Potentially, on misaligned objects like XO-3b (Hébrard et al. 2008; Winn et al. 2009) HD 80606b (Moutou et al. 2009) and CoRoT-3b, if confirmed, we could study differential rotation of stars other than the Sun.”
Determining stellar macroturbulence using asteroseismic rotational velocities from Kepler (2014, background): “…orbital axes of the planets in the Solar System are aligned to within ∼7◦ (Beck & Giles 2005), it is now known that some exoplanets c© 2014 RAS have orbits that are significantly misaligned with respect to the stellar equator (e.g. Hébrard et al. 2008; Triaud et al. 2010; Albrecht et al. 2012).”
On the tidal evolution of Hot Jupiters on inclined orbits (2009, background): “= 3.3 d ∼ P i.e. Ω ∼ n. 3 This spin–orbit misalignment has been confirmed since the submission of the present paper by Winn et al. (2009), who find that the sky–projected spin–orbit misalignment angle λ = 37.3◦±3.7◦, which is significantly smaller than that found by Hébrard et al. (2008).”
EXOPLANETARY SPIN–ORBIT ALIGNMENT: RESULTS FROM THE ENSEMBLE OF ROSSITER–MCLAUGHLIN OBSERVATIONS (2009, methodology): “; (7) Johnson et al. (2008); (8) Bouchy et al. (2008); (9) Wolf et al. (2007); (10) Narita et al. (2008); (11) Cochran et al. (2008); (12) Winn et al. (2008); (13) Winn et al. (2007b); (14) Loeillet et al. (2008); (15) Hébrard et al. (2008); (16) Joshi et al. (2009); (17) Narita et al. (2007).”
KEPLER-413B: A SLIGHTLY MISALIGNED, NEPTUNE-SIZE TRANSITING CIRCUMBINARY PLANET (2014, methodology): “One of the observations (BJD= 2456195.40345) was corrected from the 230±30 m/s blue shift due to Moon light pollution and measured thanks to the reference fiber pointed on the sky (e.g. Hébrard et al. 2008).”
ROTATION AND WINDS OF EXOPLANET HD 189733 b MEASURED WITH HIGH-DISPERSION TRANSMISSION SPECTROSCOPY (2015, methodology): “The RM e↵ect is often used to measure the projected obliquities (e.g. Hébrard et al. 2008; Albrecht et al. 2012) and for the case of HD 189733 b good alignment was found (Winn et al. 2006; Triaud et al. 2009; Collier Cameron et al. 2010).”