A Transiting Planet of a Sun-like Star

By P. McCullough, J. Stys, J. Valenti, C. Johns–Krull, K. Janes, Jim Heasley, B. A. Bye, C. Dodd, S. Fleming, A. Pinnick and 4 more. 2006

141 citations recorded by the source corpus.

A planet transits an 11th magnitude, G1 V star in the constellation Corona Borealis. We designate the planet XO-1b and the star XO-1, also known as GSC 02041-01657. XO-1 lacks a trigonometric distance; we estimate it to be 200 ± 20 pc. Of the 10 stars currently known to host extrasolar transiting planets, the star XO-1 is the most similar to the Sun in its physical characteristics: its radius is 1.0 ± 0.08 R☉, its mass is 1.0 ± 0.03 M☉, its V sin i < 3 km s-1, and its metallicity [Fe/H] is 0.015 ± 0.04. The orbital period of the planet XO-1b is 3.941534 ± 0.000027 days, one of the longer ones known. The planetary mass is 0.90 ± 0.07MJ, which is marginally larger than that of other transiting planets with periods between 3 and 4 days. Both the planetary radius and the inclination are functions of the spectroscopically determined stellar radius. If the stellar radius is 1.0 ± 0.08 R☉, then the planetary radius is 1.30 ± 0.11RJ and the inclination of the orbit is 87.°7 ± 1.°2. We have demonstrated a productive international collaboration between professional and amateur astronomers that was important to distinguishing this planet from many other similar candidates.

Subfields: Astronomy and Astrophysics, Education, Instrumentation

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Citations in the corpus

The 3.6-8.0 μm Broadband Emission Spectrum of HD 209458b: Evidence for an Atmospheric Temperature Inversion (2007, background): “Twenty one of these planets have been observed to transit their parent stars (McCullough et al. 2006; O’Donovan et al. 2006, 2007; Bakos et al. 2007a,b; Collier Cameron et al. 2007; Burke et al. 2007; Charbonneau et al. 2007a; Mandushev et al. 2007; Torres et al. 2007), allowing us to estimate not…”
Using Stellar Limb-Darkening to Refine the Properties of HD 209458b (2006, background): “There are currently five known extrasolar planets around stars bright enough for this kind of study: HD 209458b, TrES-1 (Alonso et al. 2004; Sozzetti et al. 2004), HD 149026b (Sato et al. 2005; Charbonneau et al. 2006b), HD 189733b (Bouchy et al. 2005; Bakos et al. 2006), XO-1b (McCullough et al. 20”
THE XO PLANETARY SURVEY PROJECT: ASTROPHYSICAL FALSE POSITIVES (2010, methodology): “Representative light curves from ET observations are shown in other papers (Burke et al. 2007, 2008; McCullough et al. 2006; Johns-Krull et al. 2008; Garcia-Melendo & McCullough 2009).”
The Kilodegree Extremely Little Telescope (KELT): A Small Robotic Telescope for Large‐Area Synoptic Surveys (2007, background): “These surveys have so far discovered six planets transiting bright stars (Alonso et al. 2004; Bakos et al. 2007; Cameron et al. 2007; McCullough et al. 2006; O’Donovan et al. 2006).”
Efficient identification of exoplanetary transit candidates from SuperWASP light curves (2007, background): “Among them are the three known planet host stars XO-1 (McCullough et al. 2006), WASP-1 and WASP-2 (Collier Cameron et al. 2007).”
The WASP Project and the SuperWASP Cameras (2006, background): “More recent surveys have had more success, with published transit detections reported by the Optical Gravitational Lensing Experiment (OGLE) survey (Udalski et al. 2002a, 2002b), TrES-1 (Alonso et al. 2004), HD 189733 (Bouchy et al. 2005), and, most recently, XO-1 (McCullough et al. 2006).”
Prospects for the Characterization and Confirmation of Transiting Exoplanets via the Rossiter-McLaughlin Effect (2006, background): “For XO-1, we adopt V ¼ 1:11 km s$1, b ¼ 0:12, and # ¼ 0:131 (McCullough et al. 2006; Holman et al. 2006), and find 'k ¼ 95" and 'V ¼ 0:39 km s$1 for k ¼ 0, and 'k ¼ 20" and 'V ¼ 1:8 km s$1 for k ¼ 90".”
DISCOVERY OF A TRANSITING PLANET AND EIGHT ECLIPSING BINARIES IN HATNet FIELD G205 (2009, background): “…that a candidate undergoes transits is an area where smaller telescopes can contribute, such as sophisticated facilities operated by amateurs (McCullough et al. 2006) or the network of photometric telescopes planned for the Las Cumbres Observatory Global Telescope Network (Brown et al. 2007).”
AN EFFICIENT AUTOMATED VALIDATION PROCEDURE FOR EXOPLANET TRANSIT CANDIDATES (2012, background): “Surveys designed to detect exoplanets via their transits soon followed (Alonso et al. 2004; McCullough et al. 2006; Bakos et al. 2007; Collier Cameron et al. 2007), motivated by the wealth of physical information that the light curve of a transiting planet can provide (Seager & Mallén-Ornelas…”
Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses (2008, methodology): “This was discovered to be a TEP by the XO project (McCullough et al. 2006).”
The Transit Light Curve Project. I. Four Consecutive Transits of the Exoplanet XO-1b (2006, methodology): “According to the ephemeris provided by McCullough et al. (2006), Tc(E) = 2, 453, 808.9170 [HJD] + E × (3.941534 days), (1) these transits correspond to epochs 17 through 20.”
Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, methodology): “The second planet discovered by the XO project (McCullough et al. 2006) is noteworthy for having a parent star which is very metalrich ( [ Fe H ] = 0.45) and a member of a common proper motion binary system (Burke et al. 2007).”