Abstract
We present new results derived from high-resolution optical spectra of the tau Boo system, secured in March-May 2000. The results do not show the same feature reported by Cameron et al (1999) as a candidate reflected-light signature from the planet. Together with earlier results from the 1998 and 1999 seasons, the new data yield a 99.9% upper limit on the opposition planet/star flux ratio epsilon < 3.5 x 10(-5) between 387.4 and 586.3 nm, a factor 3 deeper than the upper limit of Charbonneau et al (1999). For an assumed planet radius R-p, = 1.2 R-J, the upper limit on the mean geometric albedo is p < 0.22, 40% that of Jupiter. We find new evidence that the star's rotation is synchronised with the planet's orbital motion. Using a Monte Carlo analysis we infer that the planet's mass must lie in the range 5.5 to 10 times the mass of Jupiter.
Original language | English |
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Publisher | Unknown Publisher |
Number of pages | 3 |
Publication status | Published - 2004 |
Keywords
- EXTRASOLAR GIANT PLANETS
- 51 PEGASI
- STARS
- ANDROMEDAE
- SPECTRA