tau Boo b: Not so bright, but just as heavy
| dc.creator | Cameron, Andrew Collier | |
| dc.creator | Horne, Keith | |
| dc.creator | James, David | |
| dc.creator | Penny, Alan | |
| dc.creator | Semel, Meir | |
| dc.date | 2000-12-08 | |
| dc.date.accessioned | 2026-07-07T01:56:56Z | |
| dc.date.available | 2026-07-07T01:56:56Z | |
| dc.description | 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 percent upper limit on the opposition planet/star flux ratio epsilon<3.5E-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 Rp= 1.2 RJup, the upper limit on the mean geometric albedo is p < 0.22, 40 percent 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. | |
| dc.description | 3 pages, 2 eps sub-figures, To appear in:IAU Symp 202, eds. Penny, Artymowicz, Lagrange, Russell, `Planetary Systems in the Universe' | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0012186 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0012186 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/2189 | |
| dc.subject | Astrophysics | |
| dc.title | tau Boo b: Not so bright, but just as heavy | |
| dc.type | text |