|Exoplanet||List of exoplanets|
|Right ascension||(α)||10h 50m 34.72s|
|Declination||(δ)||−61° 57′ 25.9″|
|Semi-major axis||(a)||0.0306 ±0.0008 AU|
|Orbital period||(P)||1.689868 ±3e-06 d|
|Mass||(m)||1.14 ±0.12 MJ|
|Radius||(r)||1.18 ±0.07 RJ|
|Discovery date||14 April 2004|
|Discoverer(s)||Bouchy et al.|
|Open Exoplanet Catalogue||data|
In 2003 the Optical Gravitational Lensing Experiment (OGLE) detected periodic dimming in the star's light curve indicating a transiting, planetary-sized object. Since low-mass red dwarfs and brown dwarfs may mimic a planet radial velocity measurements were necessary to calculate the mass of the body. In 2004 the object was proved to be a new transiting extrasolar planet.
The planet has a mass 1.14 times that of Jupiter. Since the planet's inclination is known, this represents the best measured true mass of the planet, rather than simply the minimum mass as is the case when the inclination is unknown. It orbits the star (OGLE-TR-132) in an extremely close orbit, even closer than the famous planets 51 Pegasi b and HD 209458 b. The planet races around the star every 1 day 16.6 hours. The radius of the planet is only 18% larger than Jupiter's, despite the heating effect by the star. Planets of its kind are sometimes called "super-hot Jupiters".
- Bouchy, F.; et al. (2004). "Two new "very hot Jupiters" among the OGLE transiting candidates". Astronomy and Astrophysics. 421: L13–L16. arXiv: . Bibcode:2004A&A...421L..13B. doi:10.1051/0004-6361:20040170.
- Gillin, M.; et al. (2007). "The transiting planet OGLE-TR-132b revisited with new spectroscopy and deconvolution photometry". Astronomy and Astrophysics. 466 (2): 743–748. arXiv: . Bibcode:2007A&A...466..743G. doi:10.1051/0004-6361:20066367.
Media related to OGLE-TR-132 b at Wikimedia Commons
- "OGLE-TR-132 b". Exoplanets.
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