WASP-21b: a hot-Saturn exoplanet transiting a thick disc star

Bouchy, F.; Hebb, Leslie; Skillen, I.; Cameron, A. Collier; Smalley, B.; Udry, S.; Anderson, D. R.; Boisse, I.; Enoch, B.; Haswell, C. A.; Hébrard, G.; Hellier, C.; Joshi, Y. C.; Kane, Stephen R.; Maxted, P. F. L.; Mayor, M.; Moutou, C.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Simpson, E. K.; Smith, A. M. S.; Stempels, H. C.; Street, R. A.; Triaud, A. H. M. J.; West, R. G.; Wheatley, P. J.

doi:10.1051/0004-6361/201014817

Cited by 54 publications

(68 citation statements)

References 28 publications

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“…The smallest massive planet HAT-P-20b (Bakos et al 2010) orbits a host star with the strongest metallicity index [Fe/H] = 0.35. On one hand, this follows the trend observed at lower masses that planets around metal-rich stars contain more heavy elements and are therefore on average smaller (see Guillot 2008;Bouchy et al 2010). On the other hand, one would expect that the atmosphere of KOI-423b is poorer in heavy elements, hence yielding smaller opacities, and potentially, a smaller size.…”

Section: System Parameterssupporting

confidence: 74%

SOPHIE velocimetry ofKeplertransit candidates

Bouchy¹,

Bonomo²,

Santerne³

et al. 2011

A&A

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We report the strategy and results of our radial velocity follow-up campaign with the SOPHIE spectrograph (1.93-m OHP) of four transiting planetary candidates discovered by the Kepler space mission. We discuss the selection of the candidates KOI-428, KOI-410, KOI-552, and KOI-423. KOI-428 was established as a hot Jupiter transiting the largest and the most evolved star discovered so far and is described by Santerne et al. (2011, A&A, 528, A63). KOI-410 does not present radial velocity change greater than 120 m s −1 , which allows us to exclude at 3σ a transiting companion heavier than 3.4 M Jup . KOI-552b appears to be a transiting low-mass star with a mass ratio of 0.15. KOI-423b is a new transiting companion in the overlapping region between massive planets and brown dwarfs. With a radius of 1.22 ± 0.11 R Jup and a mass of 18.0 ± 0.92 M Jup , KOI-423b is orbiting an F7IV star with a period of 21.0874 ± 0.0002 days and an eccentricity of 0.12 ± 0.02. From the four selected Kepler candidates, at least three of them have a Jupiter-size transiting companion, but two of them are not in the mass domain of Jupiter-like planets. KOI-423b and KOI-522b are members of a growing population of known massive companions orbiting close to an F-type star. This population currently appears to be absent around G-type stars, possibly due to their rapid braking and the engulfment of their companions by tidal decay.

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Section: System Parameterssupporting

confidence: 74%

SOPHIE velocimetry ofKeplertransit candidates

Bouchy¹,

Bonomo²,

Santerne³

et al. 2011

A&A

Self Cite

101

143

View full text Add to dashboard Cite

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“…For example the masses of 1000 single stars, derived by Valenti et al (1998) via spectral analysis, were found to be systematically 10% larger than those derived from theoretical isochrones. A similar discrepancy was also found in the analysis of the stellar parameters of WASP-37 (Simpson et al 2011), WASP-39 , and WASP-21 (Bouchy et al 2010). Additionally, different sets of theoretical models might not perfectly agree with each other (Southworth 2010), and moreover at younger ages isochrones are closely packed A73, page 8 of 17 and a small change in T eff or ρ can have a significant effect on the derived stellar age.…”

Section: Stellar Parameterssupporting

confidence: 53%

WASP-54b, WASP-56b, and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP

Faedi

Pollacco

Barros

et al. 2013

A&A

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We present three newly discovered sub-Jupiter mass planets from the SuperWASP survey: WASP-54b is a heavily bloated planet of mass 0.636 +0.025 −0.024 M J and radius 1.653 +0.090 −0.083 R J . It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (e = 0.067 +0.033 −0.025 ) for WASP-54b. We investigated further the veracity of our detection of the eccentric orbit for WASP-54b, and we find that it could be real. However, given the brightness of WASP-54 V = 10.42 mag, we encourage observations of a secondary eclipse to draw robust conclusions on both the orbital eccentricity and the thermal structure of the planet. WASP-56b and WASP-57b have masses of 0.571 +0.034 −0.035 M J and 0.672 +0.049 −0.046 M J , respectively; and radii of 1.092 +0.035 −0.033 R J for WASP-56b and 0.916 +0.017 −0.014 R J for WASP-57b. They orbit main sequence stars of spectral type G6 every 4.67 and 2.84 days, respectively. WASP-56b and WASP-57b show no radius anomaly and a high density possibly implying a large core of heavy elements; possibly as high as ∼50 M ⊕ in the case of WASP-57b. However, the composition of the deep interior of exoplanets remains still undetermined. Thus, more exoplanet discoveries such as the ones presented in this paper, are needed to understand and constrain giant planets' physical properties.

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“…It is very similar to WASP-21b (Bouchy et al 2010), which has a similar mass (0.3 M Jup ), is also bloated (1.2 R Jup ), and also has a 4 day orbit around a G star.…”

Section: Wasp-74mentioning

confidence: 55%

THREE WASP-SOUTH TRANSITING EXOPLANETS: WASP-74b, WASP-83b, AND WASP-89b

Hellier

Anderson

Cameron

et al. 2015

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We report the discovery of three new transiting hot Jupiters by WASP-South together with the TRAPPIST photometer and the Euler/CORALIE spectrograph. WASP-74b orbits a star of V = 9.7, making it one of the brighter systems accessible to southern telescopes. It is a 0.95M Jup planet with a moderately bloated radius of 1.5 R Jup in a 2 day orbit around a slightly evolved F9 star. WASP-83b is a Saturn-mass planet at 0.3 M Jup with a radius of 1.0 R Jup . It is in a 5 day orbit around a fainter (V = 12.9) G8 star. WASP-89b is a 6 M Jup planet in a 3 day orbit with an eccentricity of e = 0.2. It is thus similar to massive, eccentric planets such as XO-3b and HAT-P-2b, except that those planets orbit F stars whereas WASP-89 is a K star. The V = 13.1 host star is magnetically active, showing a rotation period of 20.2 days, while star spots are visible in the transits. There are indications that the planet's orbit is aligned with the stellar spin. WASP-89 is a good target for an extensive study of transits of star spots.

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WASP-21b: a hot-Saturn exoplanet transiting a thick disc star

Cited by 54 publications

References 28 publications

SOPHIE velocimetry ofKeplertransit candidates

SOPHIE velocimetry ofKeplertransit candidates

WASP-54b, WASP-56b, and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP

THREE WASP-SOUTH TRANSITING EXOPLANETS: WASP-74b, WASP-83b, AND WASP-89b

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