期刊
ASTRONOMY & ASTROPHYSICS
卷 501, 期 2, 页码 785-792出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/200911749
关键词
binaries: eclipsing; stars: individual: WASP-6; planetary systems; techniques: photometric; techniques: radial velocities; techniques: spectroscopic
资金
- ESO La Silla staff
- STFC [ST/G009465/1, PP/F000057/1, PP/F000065/1, PP/D000955/1, PP/F000081/1, ST/G001987/1, ST/G002355/1, ST/F002599/1, PP/D000890/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/D000955/1, PP/F000057/1, ST/G009465/1, ST/F002599/1, PP/F000081/1, ST/G001987/1, PP/F000065/1, PP/D000890/1, ST/G002355/1] Funding Source: researchfish
We report the discovery of WASP-6b, an inflated sub-Jupiter mass planet transiting every 3.3610060(-0.0000035)(+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(p) = 0.503(-0.038)(+0.019) M(J) and radius R(p) = 1.224(-0.052)(+0.051) R(J), resulting in a density rho(p) = 0.27 +/- 0.05 rho(J). The mass and radius for the host star are M(*) = 0.88(-0.08)(+0.05) M(circle dot) and R(*) = 0.870(-0.036)(+0.025) R(circle dot). The non-zero orbital eccentricity e = 0.054(-0.015)(+0.018) that we measure suggests that the planet underwent a massive tidal heating similar to 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(-18)(+14) deg. In addition to similar published measurements, this result favors a dominant migration mechanism based on tidal interactions with a protoplanetary disk.
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