OGLE-TR-113

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OGLE-TR-113
Observation data
Epoch J2000.0
Constellation
(pronunciation)		 Carina [1]
Right ascension 10h 52m 24.40s [1]
Declination -61° 26' 48.5" [1]
Apparent magnitude (V) 14.42 [1]
Distance 4892 ly
(1500 [2] pc)
Spectral type K [3]
Other designations
none

OGLE-TR-113 is a distant magnitude 14.42 star in the star fields of the constellation Carina. Because of its distance of about 4900 light years, and location in a crowded field it was not notable in any way. Spectral type of the star is type K dwarf star, slightly cooler and less luminous than the Sun.

However, in 2002 the Optical Gravitational Lensing Experiment (OGLE) detected periodic dimming in the star's light curve indicating a transiting, planetary-sized object.[1] 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, OGLE-TR-113 b.[3]

[edit] OGLE-TR-113b

OGLE-TR-113b
Discovery
Discovered by Bouchy et al.
Discovery date 2004
Detection method Transit
Semi-major axis 0.0229 ± 0.0002 AU [4]
Eccentricity 0
Orbital period 1.4324757 ± 0.0000013 d [4]
Inclination 88.8° – 90° [4]
Physical characteristics
Mean radius 1.09 ± 0.03 RJ [4]
Mass 1.32 ± 0.19 MJ [4]

OGLE-TR-113b is an extrasolar planet orbiting the star OGLE-TR-113.

In 2002 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 1.32 times that of Jupiter. Since the planet's inclination is known, the value is exact. It orbits the star (OGLE-TR-113) 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 1.43 days. Interestingly, radius of the planet is only 9% larger than Jupiter's, despite the heating effect by the star. Planets of its kind are sometimes called "super-hot Jupiters".

[edit] References

  1. ^ a b c d e Udalski et al. (2002). "The Optical Gravitational Lensing Experiment. Planetary and Low-Luminosity Object Transits in the Carina Fields of the Galactic Disk". Acta Astronomica 52: 317–359. (web Preprint)
  2. ^ Santos et al. (2006). "Chemical abundances for the transiting planet host stars OGLE-TR-10, 56, 111, 113, 132, and TrES-1". Astronomy and Astrophysics 458: 997–1005. doi:10.1051/0004-6361:20065683. (web Preprint)
  3. ^ a b Bouchy et al. (2004). "Two new "very hot Jupiters" among the OGLE transiting candidates". Astronomy and Astrophysics 421: L13–L16. doi:10.1051/0004-6361:20040170. (web Preprint)
  4. ^ a b c d e Gillon et al. (2006). "High accuracy transit photometry of the planet OGLE-TR-113b with a new deconvolution-based method". Astronomy and Astrophysics 459: 249–255. doi:10.1051/0004-6361:20065844. (web Preprint)

[edit] External links


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