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

Hébrard, G.; Bouchy, F.; Pont, F.; Loeillet, B.; Rabus, M.; Bonfils, X.; Moutou, C.; Boisse, I.; Delfosse, X.; Desort, M.; Eggenberger, A.; Ehrenreich, D.; Forveille, T.; Lagrange, A. M.; Lovis, C.; Mayor, M.; Pepe, F.; Perrier, C.; Queloz, D.; Santos, N. C.; Ségransan, D.; Udry, S.; Vidal‐Madjar, A.

doi:10.1051/0004-6361:200810056

Cited by 215 publications

(245 citation statements)

References 43 publications

Supporting

Mentioning

238

Contrasting

Order By: Relevance

“…The value of the correlation parameter for the SOPHIE time series is also compatible with previous experience (e.g. Hébrard et al 2008). Finally, there is enough outof-transit data in the Spitzer time series to measure σ r precisely.…”

Section: Correlated Noisesupporting

confidence: 88%

See 1 more Smart Citation

Spin-orbit misalignment in the HD 80606 planetary system

Pont

Hébrard

Irwin

et al. 2009

A&A

Self Cite

View full text Add to dashboard Cite

We recently reported the photometric and spectroscopic detection of the primary transit of the 111-day-period, eccentric extra-solar planet HD 80606b, at Observatoire de Haute-Provence, France. The whole egress of the primary transit and a section of its central part were observed, allowing the measurement of the planetary radius, and evidence for a spin-orbit misalignment through the observation of the Rossiter-McLaughlin anomaly. The ingress not having been observed for this long-duration transit, uncertainties remained in the parameters of the system. We present here a refined, combined analysis of our photometric and spectroscopic data, together with further published radial velocities, ground-based photometry, and Spitzer photometry around the secondary eclipse, as well as new photometric measurements of HD 80606 acquired at Mount Hopkins, Arizona, just before the beginning of the primary transit. Although the transit is not detected in those new data, they provide an upper limit for the transit duration, which narrows down the possible behaviour of the Rossiter-McLaughlin anomaly in the unobserved part of the transit. We analyse the whole data with a Bayesian approach using a Markov-chain Monte Carlo integration on all available information. We find R p = 0.98 ± 0.03 R Jup for the planetary radius, and a total primary transit duration of 11.9 ± 1.3 h from first to fourth contact. Our analysis reinforces the hypothesis of spin-orbit misalignment in this system (alignment excluded at >95% level), with a positive projected angle between the planetary orbital axis and the stellar rotation (median solution λ ∼ 50 • ). As HD 80606 is a component of a binary system, the peculiar orbit of its planet could result from a Kozai mechanism.

show abstract

Section: Correlated Noisesupporting

confidence: 88%

“…HD 80606 is the second highly tilted planetary orbit known, after XO-3 (Hébrard et al 2008;Winn et al 2009), out of the twelve measured systems ). More strikingly, four of these planets have eccentric orbits, and two of those have tilted orbit.…”

Section: Spin-orbit Anglementioning

confidence: 94%

Spin-orbit misalignment in the HD 80606 planetary system

Pont

Hébrard

Irwin

et al. 2009

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Therefore, our general result provides further evidence for planet formation in a circumstellar disk, and suggests that the evolution of planetary systems might not lead to excitation of extreme inclinations for planetary orbits relative to the original plane of the disk. Additional evidence from observations of exoplanetary systems for planet formation in a disk and little inclination from the original plane includes the coplanarity of an exoplanet's orbit with a debris disk and the stellar spin -planet orbit alignment of a number of transiting planet systems (Winn et al 2005(Winn et al , 2006Wolf et al 2007;Winn et al 2007;Narita et al 2007;Bouchy et al 2008;Winn et al 2008;Loeillet et al 2008;Johnson et al 2008;Cochran et al 2008), although see Hébrard et al (2008) for one possible exception to this trend.…”

Section: Discussionmentioning

confidence: 99%

The architecture of the GJ 876 planetary system

Bean¹,

Seifahrt²

2009

A&A

View full text Add to dashboard Cite

We present a combined analysis of previously published high-precision radial velocities and astrometry for the GJ 876 planetary system using a self-consistent model that accounts for the planet-planet interactions. Assuming the three planets so far identified in the system are coplanar, we find that including the astrometry in the analysis does not result in a best-fit inclination significantly different than that found by Rivera and collaborators from analyzing the radial velocities alone. In this unique case, the planet-planet interactions are of such significance that the radial velocity data set is more sensitive to the inclination of the system through the dependence of the interactions on the true masses of the two gas giant planets in the system (planets b and c). The astrometry does allow determination of the absolute orbital inclination (i.e. distinguishing between i and 180 − i) and longitude of the ascending node for planet b, which allows us to quantify the mutual inclination angle between its orbit and planet c's orbit when combined with the dynamical considerations. We find that the planets have a mutual inclination Φ bc = 5.0 • +3.9 • −2.3 • . This result constitutes the first determination of the degree of coplanarity in an exoplanetary system around a normal star. That we find the two planets' orbits are nearly coplanar, like the orbits of the Solar System planets, indicates that the planets likely formed in a circumstellar disk, and that their subsequent dynamical evolution into a 2:1 mean motion resonance only led to excitation of a small mutual inclination. This investigation demonstrates how the degree of coplanarity for other exoplanetary systems could also be established using data obtained from existing facilities.

show abstract

“…Three of the 14 spectra show significant signal in the skybackground fiber, because of moonlight. This contamination was removed from CoRoT-6 spectra following the method described in Pollacco et al (2008), Barge et al (2008), and Hébrard et al (2008). This induces a significant radial velocity correction for only one measurement: −400 ± 50 m s −1 at BJD = 2 454 689.4129.…”

Section: Radial Velocity Observationsmentioning

confidence: 99%

Transiting exoplanets from the CoRoT space mission

Fridlund¹,

Hébrard

Alonso

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

The CoRoT satellite exoplanetary team announces its sixth transiting planet in this paper. We describe and discuss the satellite observations as well as the complementary ground-based observations -photometric and spectroscopic -carried out to assess the planetary nature of the object and determine its specific physical parameters. The discovery reported here is a "hot Jupiter" planet in an 8.9d orbit, 18 stellar radii, or 0.08 AU, away from its primary star, which is a solar-type star (F9V) with an estimated age of 3.0 Gyr. The planet mass is close to 3 times that of Jupiter. The star has a metallicity of 0.2 dex lower than the Sun, and a relatively high 7 Li abundance. While the light curve indicates a much higher level of activity than, e.g., the Sun, there is no sign of activity spectroscopically in e.g., the [Ca ii] H&K lines.

show abstract

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

Cited by 215 publications

References 43 publications

Spin-orbit misalignment in the HD 80606 planetary system

Spin-orbit misalignment in the HD 80606 planetary system

The architecture of the GJ 876 planetary system

Transiting exoplanets from the CoRoT space mission

Contact Info

Product

Resources

About