A Possible Spin-Orbit Misalignment in the Transiting Eccentric Planet HD 17156b

Narita, Norio; Sato, Bun’ei; Ohshima, Osamu; Winn, Joshua N.

doi:10.1093/pasj/60.2.l1

Cited by 80 publications

(66 citation statements)

References 26 publications

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“…The results are consistent with previous determinations Irwin et al 2008;Narita et al 2008;Gillon et al 2008); nevertheless the values of inclination and stellar radius show larger deviations than values presented by other authors.…”

Section: Photometric Analysissupporting

confidence: 92%

“…Our RV monitoring of HD 17156 during the 2007 December 3 transit does not confirm the misalignment between the stellar spin and planet orbit axes claimed by Narita et al (2008), but it agrees instead with the opposite finding by Cochran et al (2008). We think our results are more robust because the other most accurate dataset (HET in Cochran et al 2008) does not cover the full transit, leaving some uncertainties in their Rossiter modeling.…”

Section: Summary and Discussioncontrasting

confidence: 77%

“…In their analysis Irwin et al (2008) and Narita et al (2008) fixed the stellar radius to the value proposed by F07, while Gillon et al (2008) directly obtained the radius from their analysis. The origin of the discrepancy of the stellar radius might lie in the different values for the inclination, because its value controls the transit duration and the relative sum of the radii.…”

Section: Photometric Analysismentioning

confidence: 99%

“…Additional photometric measurements were presented in followup papers by Gillon et al (2008), Narita et al (2008), Irwin et al (2008), Winn et al (2008). This planet is unique among the known transiting systems in that its period (21.2 days) is more Article published by EDP Sciences than 5 times longer than the average period for this sample, and it has the largest eccentricity (e = 0.67).…”

Section: Introductionmentioning

confidence: 99%

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Characterization of the HD 17156 planetary system

Barbieri¹,

Alonso²,

Desidera

et al. 2009

A&A

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Aims. We present data to improve the known parameters of the HD 17156 system (peculiar due to the eccentricity and long orbital period of its transiting planet) and constrain the presence of stellar companions. Methods. Photometric data were acquired for 4 transits, and high precision radial velocity measurements were simultaneously acquired with the SARG spectrograph at TNG for one transit. The template spectra of HD 17156 was used to derive effective temperature, gravity, and metallicity. A fit of the photometric and spectroscopic data was performed to measure the stellar and planetary radii, and the spin-orbit alignment. Planet orbital elements and ephemeris were derived from the fit. Near infrared adaptive optic images were acquired with the AdOpt module of TNG. Results. We found that the star has a radius of R S = 1.44 ± 0.03 R and the planet R P = 1.02 ± 0.08 R J . The transit ephemeris is T c = 2 454 756.73134 ± 0.00020 + N · 21.21663 ± 0.00045 BJD. Analysis of the Rossiter-Mclaughlin effect shows that the system is spin orbit aligned with an angle β = 4.8 • ± 5.3 • . The analysis of high resolution images did not reveal any stellar companion with a projected separation between of 150 and 1 000 AU from HD 17156.

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Section: Photometric Analysissupporting

confidence: 92%

Section: Summary and Discussioncontrasting

confidence: 77%

Section: Photometric Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Characterization of the HD 17156 planetary system

Barbieri¹,

Alonso²,

Desidera

et al. 2009

A&A

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“…The RME has been shown to be a powerful tool for transiting planets as well. The method has been applied for measuring of the spin-orbit alignment for eleven of the transiting planets (Bundy & Marcy 2000;Queloz et al 2000;Winn et al 2005Winn et al , 2006Winn et al , 2007Narita et al 2007;Wolf et al 2007;Bouchy et al 2008;Cochran et al 2008;Hébrard et al 2008;Johnson et al 2008;Joshi et al 2008;Loeillet et al 2008;Narita et al 2008). With the fast-growing number of bright Article published by EDP Sciences host stars of transiting planets, either from ground-based widefield surveys or from space missions, this measurement turns into a standard tool for investigating the properties of extrasolar planets.…”

Section: Introductionmentioning

confidence: 99%

On the possibility of detecting extrasolar planets' atmospheres with the Rossiter-McLaughlin effect

Reiners

Homeier

Noll

2009

A&A

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Context. The detection of extrasolar planets' atmospheres requires very demanding observations. For planets that cannot be spatially separated from their host stars, i.e. the vast majority of planets, the transiting planets are the only ones to allow their atmospheres to be probed. This is possible from transmission spectroscopy or from measurements taken during the secondary eclipse. An alternative is to measure of the Rossiter-McLaughlin effect, which is sensitive to the size of the planetary radius. Since the radius is wavelengthdependent due to contributions of strong planetary absorption lines, this opens a path toward also probing planetary atmospheres with ground-based high-resolution spectroscopy. Aims. The major goal of our numerical simulations is to provide a reliable estimate of the amplitude of the wavelength-dependent Rossiter-McLaughlin effect. Methods. Our numerical simulations provide detailed phase-resolved synthetic spectra modeling the partly eclipsed stellar surface during the transit. With these spectra we can obtain Rossiter-McLaughlin curves for different wavelength regions and for a wavelengthdependent planetary radius. Curves from regions with high and low contributions of absorption lines within the planetary atmosphere can be compared. Observable quantities are derived from these differential effects.Results. We applied our simulations to HD 209458. Our numerical simulations show that a detailed treatment of the limb-darkening for the synthetic spectra is important for a precise analysis. Compared to a parameterized limb-darkening law, systematic errors of 6 m s −1 occur. The wavelength dependency of the planetary atmospheres over the NaD-doublet produces a differential effect in the Rossiter-McLaughlin curve of 1.5 m s −1 for a star with a rotation velocity of 4.5 km s −1 , which increases to 4 m s −1 for twice the rotation velocity. Conclusions. As a tool for probing planetary atmospheres the Rossiter-McLaughlin effect requires phase-resolved, high signal-tonoise, high-resolution spectra taken with a stabilized spectrograph in order to obtain reliable results for slowly rotating (<10 m s −1 ) planet host stars. Stars with spectral type earlier than about F5 are a bit less demanding since the typically higher rotation velocity increases the amplitude of the effect to about 15 m s −1 for a star with v sin i = 25 km s −1 .

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Exoplanet Observations

Bean

2010

Formation and Evolution of Exoplanets

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A Possible Spin-Orbit Misalignment in the Transiting Eccentric Planet HD 17156b

Cited by 80 publications

References 26 publications

Characterization of the HD 17156 planetary system

Characterization of the HD 17156 planetary system

On the possibility of detecting extrasolar planets' atmospheres with the Rossiter-McLaughlin effect

Exoplanet Observations

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