The retrograde orbit of the HAT-P-6b exoplanet

Hébrard, G.; Ehrenreich, D.; Bouchy, F.; Delfosse, X.; Moutou, C.; Arnold, L.; Boisse, I.; Bonfils, X.; Díaz, R. F.; Eggenberger, A.; Forveille, T.; Lagrange, Anne-Marie; Lovis, C.; Pepe, F.; Perrier, C.; Queloz, D.; Santerne, A.; Santos, N. C.; Ségransan, D.; Udry, S.; Vidal‐Madjar, A.

doi:10.1051/0004-6361/201016331

Cited by 88 publications

(89 citation statements)

References 51 publications

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“…Each of them has some peculiarities, however, WASP-52b and WASP-58b are new cases of inflated planets, increasing the population of giant planets with abnormally large radii whose origin is not well understood yet despite the numerous models proposed to explain them (see, e.g., Fortney & Nettelmann 2010). WASP-52 is a new case of a possibly slightly misaligned system; it does not fit with the possible correlations of λ with T eff (Winn et al 2010) or M p (Hébrard et al 2011), however. The hot Jupiter WASP-58b orbits a particularly metal-poor star.…”

Section: Resultsmentioning

confidence: 99%

WASP-52b, WASP-58b, WASP-59b, and WASP-60b: Four new transiting close-in giant planets

Hébrard

Cameron

Brown

et al. 2013

A&A

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We present the discovery of four new transiting hot Jupiters, detected mainly from SuperWASP-North and SOPHIE observations. These new planets, WASP-52b, WASP-58b, WASP-59b, and WASP-60b, have orbital periods ranging from 1.7 to 7.9 days, masses between 0.46 and 0.94 M Jup , and radii between 0.73 and 1.49 R Jup . Their G1 to K5 dwarf host stars have V magnitudes in the range 11.7−13.0. The depths of the transits are between 0.6 and 2.7%, depending on the target. With their large radii, WASP-52b and WASP-58b are new cases of low-density, inflated planets, whereas WASP-59b is likely to have a large, dense core. WASP-60 shows shallow transits. In the case of WASP-52 we also detected the Rossiter-McLaughlin anomaly via time-resolved spectroscopy of a transit. We measured the sky-projected obliquity λ = 24 • +17 −9 , indicating that WASP-52b orbits in the same direction as its host star is rotating and that this prograde orbit is slightly misaligned with the stellar equator. These four new planetary systems increase our statistics on hot Jupiters and provide new targets for follow-up studies.

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Section: Resultsmentioning

confidence: 99%

WASP-52b, WASP-58b, WASP-59b, and WASP-60b: Four new transiting close-in giant planets

Hébrard

Cameron

Brown

et al. 2013

A&A

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119

153

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“…However, exo-planets with strong spin-orbit misalignment have been detected (e.g. β > 50 • ; Moutou et al 2011a,b;Hébrard et al 2011;Simpson et al 2011). Considering that the plane of the past protoplanetary disc should be identical to the present stellar equator 1 , the orbital plane of these planets must have been changed by some mechanism.…”

Section: Introductionmentioning

confidence: 99%

Highly inclined and eccentric massive planets

Bitsch

Crida

Libert

et al. 2013

A&A

117

187

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Context. In the solar system, planets have a small inclination with respect to the equatorial plane of the Sun, but there is evidence that in extrasolar systems the inclination can be very high. This spin-orbit misalignment is unexpected, as planets form in a protoplanetary disc supposedly aligned with the stellar spin. It has been proposed that planet-planet interactions can lead to mutual inclinations during migration in the protoplanetary disc. However, the effect of the gas disc on inclined giant planets is still unknown. Aims. In this paper we investigate planet-disc interactions for planets above 1 M Jup . We check the influence of three parameters: the inclination i, eccentricity e, and mass M p of the planet. This analysis also aims at providing a general expression of the eccentricity and inclination damping exerted on the planet by the disc. Methods. We perform three-dimensional numerical simulations of protoplanetary discs with embedded high-mass planets on fixed orbits. We use the explicit/implicit hydrodynamical code NIRVANA in 3D with an isothermal equation of state. Results. We provide damping formulae for i and e as a function of i, e, and M p that fit the numerical data. For highly inclined massive planets, the gap opening is reduced, and the damping of i occurs on time-scales of the order of 10 −4 deg/year · M disc /(0.01 M ) with the damping of e on a smaller time-scale. While the inclination of low planetary masses (<5 M Jup ) is always damped, large planetary masses with large i can undergo a Kozai-cycle with the disc. These Kozai-cycles are damped through the disc in time. Eccentricity is generally damped, except for very massive planets (M p ∼ 5 M Jup ) where eccentricity can increase for low inclinations. So the dynamics tends to a final state: planets end up in midplane and can then, over time, increase their eccentricity as a result of interactions with the disc. Conclusions. The interactions with the disc lead to damping of i and e after a scattering event of high-mass planets. If i is sufficiently reduced, the eccentricity can be pumped up because of interactions with the disc. If the planet is scattered to high inclination, it can undergo a Kozai-cycle with the disc that makes it hard to predict the exact movement of the planet and its orbital parameters at the dispersal of the disc.

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“…About thirty misaligned systems (|λ| > 30 • and inconsistent with λ = 0 • ) have been identified, over more than eighty measured systems 1 (Albrecht et al 2012;Crida & Batygin 2014), including some with retrograde or nearly polar orbits (e.g., Winn et al 2009;Narita et al 2010;Triaud et al 2010;Hébrard et al 2011). Most of these measurements have been done for close-in, isolated giant planets.…”

Section: Introductionmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Bourrier

Étangs

Hébrard

et al. 2015

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We present the detection and characterization of the transiting warm Jupiter KOI-12b, first identified with Kepler with an orbital period of 17.86 days. We combine the analysis of Kepler photometry with Doppler spectroscopy and line-profile tomography of timeseries spectra obtained with the SOPHIE spectrograph to establish its planetary nature and derive its properties. To derive reliable estimates for the uncertainties on the tomographic model parameters, we devised an empirical method of calculating statistically independent error bars on the time-series spectra. KOI-12b has a radius of 1.43 ± 0.13 R Jup and a 3σ upper mass limit of 10 M Jup . It orbits a fast-rotating star (v sin i = 60.0 ± 0.9 km s −1 ) with mass and radius of 1.45 ± 0.09 M and 1.63 ± 0.15 R , located at 426 ± 40 pc from the Earth. Doppler tomography allowed higher precision on the obliquity to be reached by comparison with analysis of the Rossiter-McLaughlin radial velocity anomaly, and we find that KOI-12b lies on a prograde, slightly misaligned orbit with low sky-projected obliquity λ = 12.6 +3.0 −2.9• . The properties of this planetary system, with a 11.4 mag host star, make of KOI-12b a precious target for future atmospheric characterization.

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The retrograde orbit of the HAT-P-6b exoplanet

Cited by 88 publications

References 51 publications

WASP-52b, WASP-58b, WASP-59b, and WASP-60b: Four new transiting close-in giant planets

WASP-52b, WASP-58b, WASP-59b, and WASP-60b: Four new transiting close-in giant planets

Highly inclined and eccentric massive planets

SOPHIE velocimetry ofKeplertransit candidates

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