Mass of WASP-33b

Lehmann, H.; Guenther, E. W.; Sebastian, Daniel; Döllinger, M. P.; Hartmann, Michael; Mkrtichian, D. E.

doi:10.1051/0004-6361/201526176

Cited by 37 publications

(33 citation statements)

References 28 publications

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“…We used a mean molecular weight of Article number, page 3 of 12 A&A proofs: manuscript no. CaII-paper-acc Lehmann et al (2015) with parameters form Kovács et al (2013). b Adopted from Johnson et al (2015).…”

Section: Cross-correlation With Simulated Templatementioning

confidence: 99%

Ionized calcium in the atmospheres of two ultra-hot exoplanets WASP-33b and KELT-9b

Yan

Casasayas-Barris

Molaverdikhani

et al. 2019

A&A

133

132

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Ultra-hot Jupiters are emerging as a new class of exoplanets. Studying their chemical compositions and temperature structures will improve the understanding of their mass loss rate as well as their formation and evolution. We present the detection of ionized calcium in the two hottest giant exoplanets -KELT-9b and WASP-33b. By utilizing transit datasets from CARMENES and HARPS-N observations, we achieved high confidence level detections of Ca ii using the cross-correlation method. We further obtain the transmission spectra around the individual lines of the Ca ii H&K doublet and the near-infrared triplet, and measure their line profiles. The Ca ii H&K lines have an average line depth of 2.02 ± 0.17 % (effective radius of 1.56 R p ) for WASP-33b and an average line depth of 0.78 ± 0.04 % (effective radius of 1.47 R p ) for KELT-9b, which indicates that the absorptions are from very high upper atmosphere layers close to the planetary Roche lobes. The observed Ca ii lines are significantly deeper than the predicted values from the hydrostatic models. Such a discrepancy is probably a result of hydrodynamic outflow that transports a significant amount of Ca ii into the upper atmosphere. The prominent Ca ii detection with the lack of significant Ca i detection implies that calcium is mostly ionized in the upper atmospheres of the two planets.

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Section: Cross-correlation With Simulated Templatementioning

confidence: 99%

Ionized calcium in the atmospheres of two ultra-hot exoplanets WASP-33b and KELT-9b

Yan

Casasayas-Barris

Molaverdikhani

et al. 2019

A&A

133

132

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“…A few other transiting hot Jupiters have been found around such hot and fast rotating stars (Table 7). CoRoT-11, WASP-33, and KELT-7 have been observed extensively in radial velocities, with 31, 248, and 36 measurements along the orbit respectively, yielding the planets' masses (Gandolfi et al 2010;Lehmann et al 2015;Bieryla et al 2015). CoRoT-3b is so massive that the recoil motion overwhelms stellar rotation effects (Deleuil et al 2008).…”

Section: Stellar Parametersmentioning

confidence: 99%

Discovery of XO-6b: A Hot Jupiter Transiting a Fast Rotating F5 Star on an Oblique Orbit

Crouzet¹,

McCullough²,

Long³

et al. 2017

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Only a few hot Jupiters are known to orbit around fast rotating stars. These exoplanets are harder to detect and characterize and may be less common than around slow rotators. Here, we report the discovery of the transiting hot Jupiter XO-6b, which orbits a bright, hot, and fast rotating star: V = 10.25, T ef f = 6720 ± 100 K, v sin i = 48 ± 3 km s −1 . We detected the planet from its transits using the XO instruments and conducted a follow-up campaign. Because of the fast stellar rotation, radial velocities taken along the orbit do not yield the planet's mass with a high confidence level, but we secure a 3-σ upper limit M p < 4.4 M Jup . We also obtain high resolution spectroscopic observations of the transit with the SOPHIE spectrograph at the 193-cm telescope of the Observatoire de Haute-Provence and analyze the stellar lines profile by Doppler tomography. The transit is clearly detected in the spectra. The radii measured independently from the tomographic analysis and from the photometric lightcurves are consistent, showing that the object detected by both methods is the same and indeed transits in front of XO-6. We find that XO-6b lies on a prograde and misaligned orbit with a skyprojected obliquity λ = −20.7• ± 2.3• . The rotation period of the star is shorter than the orbital period of the planet: P rot < 2.12 days, P orb = 3.77 days. Thus, this system stands in a largely unexplored regime of dynamical interactions between close-in giant planets and their host stars.

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“…WASP-33b is a 2.2 M J planet with a radius of 1.5 R J orbiting a 1.5 M Sun δ Scuti star with a period of 1.22 days (Lehmann et al 2015). With an irradiation temperature ( * = T T a 0 e f f ) of 3890 K, this planet is one of the most highly irradiated hot Jupiters currently known.…”

Section: Introductionmentioning

confidence: 99%

Phase Curves of WASP-33b and HD 149026b and a New Correlation between Phase Curve Offset and Irradiation Temperature

et al. 2018

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We present new 3.6 and 4.5 μm Spitzer phase curves for the highly irradiated hot Jupiter WASP-33b and the unusually dense Saturn-mass planet HD 149026b. As part of this analysis, we develop a new variant of pixel-level decorrelation that is effective at removing intrapixel sensitivity variations for long observations (>10 hr) where the position of the star can vary by a significant fraction of a pixel. Using this algorithm, we measure eclipse depths, phase amplitudes, and phase offsets for both planets at 3.6 and 4.5 μm. We use a simple toy model to show that WASP-33b's phase offset, albedo, and heat recirculation efficiency are largely similar to those of other hot Jupiters despite its very high irradiation. On the other hand, our fits for HD 149026b prefer a very high albedo. We also compare our results to predictions from general circulation models, and we find that while neither planet matches the models well, the discrepancies for HD 149026b are especially large. We speculate that this may be related to its high bulk metallicity, which could lead to enhanced atmospheric opacities and the formation of reflective cloud layers in localized regions of the atmosphere. We then place these two planets in a broader context by exploring relationships between the temperatures, albedos, heat transport efficiencies, and phase offsets of all planets with published thermal phase curves. We find a striking relationship between phase offset and irradiation temperature: the former drops with increasing temperature until around 3400 K and rises thereafter. Although some aspects of this trend are mirrored in the circulation models, there are notable differences that provide important clues for future modeling efforts.

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Mass of WASP-33b

Cited by 37 publications

References 28 publications

Ionized calcium in the atmospheres of two ultra-hot exoplanets WASP-33b and KELT-9b

Ionized calcium in the atmospheres of two ultra-hot exoplanets WASP-33b and KELT-9b

Discovery of XO-6b: A Hot Jupiter Transiting a Fast Rotating F5 Star on an Oblique Orbit

Phase Curves of WASP-33b and HD 149026b and a New Correlation between Phase Curve Offset and Irradiation Temperature

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