The Spectroscopic Orbit of the Planetary Companion Transiting HD 209458

Abstract

We report a spectroscopic orbit with period days for the planetary companion that P = 3.52433 ‫ע‬ 0.00027 transits the solar-type star HD 209458. For the metallicity, mass, and radius of the star, we derive [Fe/H] = , , and . This is based on a new analysis of the iron lines in 0.00 ‫ע‬ 0.02our HIRES template spectrum and also on the absolute magnitude, effective temperature, and color of the star, and it uses isochrones from four different sets of stellar evolution models. Using these values for the stellar parameters, we reanalyze the transit data and derive an orbital inclination of .

Planetary transit observations at the University Observatory Jena: XO‐1b and TrES‐1

“…In the last ten years a further indirect detection method has established itself as a highly successful technique in finding and confirming planets -the transit method. The first success of this technique was the confirmation of the planet candidate HD 209458b, which was found by the radial velocity method (Mazeh et al 2000), as a real planet by Charbonneau et al (2000). Since that time more than 50 transiting planets have been discovered by over 20 ground-based projects and space missions.…”

The atmospheres of extrasolar planets

“…The most extreme example is HD 209458 b, with an average density of -0.35 g/cm2. This planet was the first one found to exhibit a transit (Charbonneau et al, 2000;Henry et al, 2000), although it was originally detected using the radial velocity method (Mazeh et al, 2000). Since then, it has been observed extensively from the ground and from space, as we shall discuss further in Section 2.7.…”

New Insights into Extrasolar Giant Planets

“…Defined as objects found using the high-precision radial-velocity technique around stars with little or no intrinsic variability and previously thought to be without companions, the rv60 extrasolar giant planets (EGPs; Burrows et al 1995) that have been discovered to date span more than two orders of magnitude in mpsin(i), semi-major axis, and period Cochran et al 1997;Delfosse et al 1998;Fischer et al 1999;Henry et al 2000;Korzennik et al 2000;Latham et al 1989;Marcy and Butler 1996;Marcy et al 1999;Marcy, Butler, and Vogt 2000;Marcy, Cochran, and Major 2000;Mayor and Queloz 1995;Mazeh et al 2000;Noyes et al 1997;Queloz et al 2000;Santos et al 2000;Ddry et al 2000;Vogt et al 2000;and references therein). Collectively, EGPs show the wide range of eccentricities typical of stellar companions, while those within rvO.07 A.D. have the small eccentricities expected for objects that have experienced significant tidal dissipation.…”

“…Although the brown dwarf Gliese 229B is 10-50 times as massive as the EGP 51 Peg b, they have similar effective temperatures. Moreover, stellar irradiation can swell the radii of such short-period gas giants by 20% to 80%, thereby enhancing the magnitude and probability of the photometric dip during a planetary transit (e.g., HD209458b: Charbonneau et al 1999, Henry et al 2000Mazeh et al 2000, Jha et al 2000.…”

“…The ingress and egress phases each last ",,25 minutes Henry et al 2000). The properties of the planet, in particular its orbital distance and radius, scale with the properties of the star and values for the planet's radius (R p ) around ""1.4 RJ have been quoted (Henryet al 2000;Charbonneau et al 2000;Mazeh et al 2000;Jha et al 2000), with the most precise value, 1.347 ± 0.060RJ, derived from HST/STIS photometry .…”