Spin-orbit misalignment in the HD 80606 planetary system

Pont, F.; Hébrard, G.; Irwin, Jonathan; Bouchy, F.; Moutou, C.; Ehrenreich, D.; Guillot, T.; Aigrain, S.; Bonfils, X.; Berta, Zachory K.; Boisse, I.; Burke, Christopher J.; Charbonneau, D.; Delfosse, X.; Desort, M.; Eggenberger, A.; Forveille, T.; Lagrange, A. M.; Lovis, C.; Nutzman, P.; Pepe, F.; Perrier, C.; Queloz, D.; Santos, N. C.; Ségransan, D.; Udry, S.; Vidal‐Madjar, A.

doi:10.1051/0004-6361/200912463

Cited by 78 publications

(91 citation statements)

References 27 publications

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“…When combining the 26 RM effects that have been observed, we now see that eight planets are severely misaligned: XO-3b (Hébrard et al 2008;Winn et al 2009c), HD 80606b Pont et al 2009;Winn et al 2009a), WASP-14b (Johnson et al 2009), Hat-P-7b (Winn et al 2009b;Narita et al 2009), WASP-8b ) and WASP-2b, WASP15b and WASP17b. Of these eight, five have been found to be in retrograde orbits, four from our survey.…”

Section: Discussionmentioning

confidence: 72%

Spin-orbit angle measurements for six southern transiting planets

Triaud

Cameron

Queloz

et al. 2010

A&A

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Context. Several competing scenarios for planetary-system formation and evolution seek to explain how hot Jupiters came to be so close to their parent stars. Most planetary parameters evolve with time, making it hard to distinguish between models. The obliquity of an orbit with respect to the stellar rotation axis is thought to be more stable than other parameters such as eccentricity. Most planets, to date, appear aligned with the stellar rotation axis; the few misaligned planets so far detected are massive (>2 M J ). Aims. Our goal is to measure the degree of alignment between planetary orbits and stellar spin axes, to search for potential correlations with eccentricity or other planetary parameters and to measure long term radial velocity variability indicating the presence of other bodies in the system. Methods. For transiting planets, the Rossiter-McLaughlin effect allows the measurement of the sky-projected angle β between the stellar rotation axis and a planet's orbital axis. Using the HARPS spectrograph, we observed the Rossiter-McLaughlin effect for six transiting hot Jupiters found by the WASP consortium. We combine these with long term radial velocity measurements obtained with CORALIE. We used a combined analysis of photometry and radial velocities, fitting model parameters with the Markov Chain Monte Carlo method. After obtaining β we attempt to statistically determine the distribution of the real spin-orbit angle ψ. Results. We found that three of our targets have β above 90 • : WASP-2b: β = 153 • +11 −15 , WASP-15b: β = 139.6 • +5.2 −4.3 and WASP17b: β = 148.5 • +5.1 −4.2 ; the other three (WASP-4b, WASP-5b and WASP-18b) have angles compatible with 0 • . We find no dependence between the misaligned angle and planet mass nor with any other planetary parameter. All six orbits are close to circular, with only one firm detection of eccentricity e = 0.00848 +0.00085 −0.00095 in WASP-18b. No long-term radial acceleration was detected for any of the targets. Combining all previous 20 measurements of β and our six and transforming them into a distribution of ψ we find that between about 45 and 85% of hot Jupiters have ψ > 30 • . Conclusions. Most hot Jupiters are misaligned, with a large variety of spin-orbit angles. We find observations and predictions using the Kozai mechanism match well. If these observational facts are confirmed in the future, we may then conclude that most hot Jupiters are formed from a dynamical and tidal origin without the necessity to use type I or II migration. At present, standard disc migration cannot explain the observations without invoking at least another additional process.

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Section: Discussionmentioning

confidence: 72%

Spin-orbit angle measurements for six southern transiting planets

Triaud

Cameron

Queloz

et al. 2010

A&A

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“…The exoplanet with the largest well-determined eccentricity is HD 80606b; e=0.9332 and the remarkably small a=0.449 AU (Naef et al 2001;Pont et al 2009). These same authors offered several suggestions for the origin of HD 80606bʼs orbit, including the gravitational interaction with another planet(s), especially if that other planet were expelled in a violent interaction.…”

Section: Comparison With Known Extreme Exoplanetsmentioning

confidence: 98%

Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Shara

Hurley

Mardling

2016

ApJ

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Explaining the origin and evolution of exoplanetary hot Jupiters remains a significant challenge. One possible mechanism for the production of hot Jupitersis planet-planet interactions, which produce them from planets born far from their host stars but near their dynamical stability limits. In the much more likely case of planets born far from their dynamical stability limits, can hot Jupiters be formed in star clusters? Our N-body simulations answer this question in the affirmative, and show that hot Jupiter formation is not a rare event, occurring in ∼1% of star cluster planetary systems. We detail three case studies of the dynamics-induced births of hot Jupiters on highly eccentric orbits that can only occur inside star clusters. The hot Jupiters' orbits bear remarkable similarities to those of some of the most extreme exoplanets known: HAT-P-32b, HAT-P-2b, HD 80606b, and GJ 876d. If stellar perturbations formed these hot Jupiters, then our simulations predict that these very hot inner planets are often accompanied by much more distant gas giants in highly eccentric orbits.

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“…A thorough analysis of the collected data around the February 2009 primary transit led to the conclusion that there is a significant spin-orbit misalignment in the system, i.e. the orbital plane of HD 80606b fails to coincide with the equatorial plane of its host star (Pont et al 2009). These facts suggest that this planet might be seen at an instant close to the maximum eccentricity phase of a Kozai cycle induced by a distant, inclined third companion (cf.…”

Section: Figmentioning

confidence: 99%

Transit timing variations in eccentric hierarchical triple exoplanetary systems

Borkovits

Csizmadia

Forgács‐Dajka

et al. 2011

A&A

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Aims. We study the long-term time scale (i.e. period comparable to the orbital period of the outer perturber object) transit timing variations (TTVs) in transiting exoplanetary systems that contain another more distant (a 2 a 1 ) planetary or stellar companion. Methods. We give an analytical form of the O−C diagram (which describes such TTVs) in a trigonometric series, which is valid for arbitrary mutual inclinations, up to the sixth order in the inner eccentricity. Results. We show that the dependence of the O−C on the orbital and physical parameters can be separated into three parts. Two of these are independent of the real physical parameters (i.e. masses, separations, periods) of a concrete system and only depend on dimensionless orbital elements, so can be analysed in general. We find that, for a specific transiting system, where eccentricity (e 1 ) and the observable argument of periastron (ω 1 ) are known, say, from spectroscopy, the main characteristics of that TTV, which is caused by a possible third-body can be mapped simply. Moreover, as the physical attributes of a given system only occur as scaling parameters, the real amplitude of the O−C can also be estimated for a given system, simply as a function of the m 3 /P 2 ratio. We analyse the above-mentioned dimensionless amplitudes for different arbitrary initial parameters, as well as for two particular systems, CoRoT-9b and HD 80606b. We find in general that, while the shape of the O−C strongly varies with the angular orbital elements, the net amplitude (departing from some specific configurations) depends only weakly on these elements, but strongly on the eccentricities. As an application, we illustrate how the formulae work for the weakly eccentric CoRoT-9b and the highly eccentric HD 80606b. We also consider the question of detection, as well as the correct identification of such perturbations. Finally, we illustrate the operation and effectiveness of Kozai cycles with tidal friction (KCTF) in the case of HD 80606b.

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Spin-orbit misalignment in the HD 80606 planetary system

Cited by 78 publications

References 27 publications

Spin-orbit angle measurements for six southern transiting planets

Spin-orbit angle measurements for six southern transiting planets

Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Transit timing variations in eccentric hierarchical triple exoplanetary systems

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