HD 80606 b, a planet on an extremely elongated orbit

Naef, D.; Latham, David W.; Mayor, M.; Mazeh, T.; Beuzit, Jean-Luc; Drukier, G. A.; Perrier-Bellet, C.; Queloz, D.; Sivan, J. P.; Torres, Guillermo; Udry, S.; Zucker, S.

doi:10.1051/0004-6361:20010853

Cited by 206 publications

(201 citation statements)

References 25 publications

Supporting

Mentioning

195

Contrasting

Order By: Relevance

“…Other known transiting objects with long periods are WASP-8b with P = 8.16 days, M = 2.23 M Jup (Smith et al 2009), CoRoT-4b with P = 9.20 days, M = 0.72 M Jup (Aigrain et al 2008), and HD 17156b with P = 21.22 days, M = 3.21 M Jup , (Barbieri et al 2007;Fischer et al 2007). There is also the case of HD 80606b with P = 111.43 days, M = 3.94 M Jup (Naef et al 2001). Thus, of the 5 transiting objects with periods longer than 8 days, 4 have masses of between 2 and 4 M Jup , and only one -CoRoT-4b -is a somewhat smaller object of M = 0.72 M Jup .…”

Section: Planetary Parametersmentioning

confidence: 91%

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

Section: Planetary Parametersmentioning

confidence: 91%

Transiting exoplanets from the CoRoT space mission

Fridlund¹,

Hébrard

Alonso

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

“…Some of the hot Jupiters appear to be in multiple systems but this appears unrelated to other parameters such as eccentricity or misalignment. Examples are: HD 80606 (Naef et al 2001), HD 189733 (Bakos et al 2006), Hat-P-1 (Bakos et al 2007), WASP-8 (Queloz et al 2010), Hat-P-7 (Winn et al 2009b), WASP-2, TrES-2 and TrES-4 (Daemgen et al 2009). …”

Section: Correlations Between Parametersmentioning

confidence: 99%

Spin-orbit angle measurements for six southern transiting planets

Triaud

Cameron

Queloz

et al. 2010

A&A

Self Cite

431

440

View full text Add to dashboard Cite

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.

show abstract

HD 80606 b, a planet on an extremely elongated orbit

Cited by 206 publications

References 25 publications

Transiting exoplanets from the CoRoT space mission

Transiting exoplanets from the CoRoT space mission

Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Spin-orbit angle measurements for six southern transiting planets

Contact Info

Product

Resources

About