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Discovery and characterization of WASP-6b, an inflated sub-Jupiter mass planet transiting a solar-type star

By M. Gillon, D. R. Anderson, A. H. M. J. Triaud, Coel Hellier, Pierre Maxted, Don Pollacco, Didier Queloz, Barry Smalley, Richard G. West, D. M. (David M.) Wilson, Samuel J. Bentley, A. Collier Cameron, B. Enoch, L. Hebb, K. (Keith) Horne, Jonathan Irwin, Y. C. Joshi, T. A. Lister, M. (Michel) Mayor, Francesco Pepe, N. Parley, D. Segransan, S. Udry and P. J. Wheatley


We report the discovery of WASP-6b, an inflated sub-Jupiter mass planet transiting every $ 3.3610060^{\rm + 0.0000022 }_ $ days a mildly metal-poor solar-type star of magnitude V = 11.9. A combined analysis of the WASP photometry, high-precision followup transit photometry and radial velocities yield a planetary mass $M_{\rm p} = 0.503^_$ $M_{\rm J}$ and radius $R_{\rm p} = 1.224^_$ $R_{\rm J}$, resulting in a density $\rho_{\rm p} = 0.27 \pm 0.05$ $\rho_{\rm J}$. The mass and radius for the host star are $M_\ast = 0.88^_$ $M_\odot$ and $R_\ast = 0.870^_$ $R_\odot$. The non-zero orbital eccentricity $e = 0.054^{\rm +0.018}_$ that we measure suggests that the planet underwent a massive tidal heating ~1 Gyr ago that could have contributed to its inflated radius. High-precision radial velocities obtained during a transit allow us to measure a sky-projected angle between the stellar spin and orbital axis $\beta = 11^_$ deg. In addition to similar published measurements, this result favors a dominant migration mechanism based on tidal interactions with a protoplanetary disk

Topics: QB
Publisher: EDP Sciences
Year: 2009
OAI identifier:

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