OGLE-TR-132

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OGLE-TR-132
Observation data
Epoch J2000.0
Constellation
(pronunciation)		 Carina [1]
Right ascension 10h 50m 34.72s [1]
Declination -61° 57' 25.9" [1]
Apparent magnitude (V) 15.72 [1]
Distance 4892 ly
(1500 [2] pc)
Spectral type F [3]
Other designations
none

OGLE-TR-132 is a distant magnitude 15.72 star in the star fields of the constellation Carina. Because of its great distance, about 4900 light years, and location in the crowded field it was not notable in any way. Spectral type of the star is type F yellow-white very metal rich dwarf star, slightly hotter and more luminous than the Sun.

However, in 2003 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-132 b.[3]

[edit] OGLE-TR-132b

OGLE-TR-132b
Discovery
Discovered by Bouchy et al.
Discovery date 2004
Detection method Transit
Semi-major axis 0.0306 ± 0.0008 AU [3]
Eccentricity 0
Orbital period 1.689868 ± 0.000003 d[4]
Inclination 85 ± 1.0°
Angular distance 0.02 mas
Physical characteristics
Mean radius 1.18 ± 0.07 RJ[4]
Mass 1.14 ± 0.12 MJ[4]

OGLE-TR-132b is an extrasolar planet orbiting the star OGLE-TR-132.

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, the value is exact. 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. Interestingly, 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".

[edit] References

  1. ^ a b c d e Udalski et al. (2003). "The Optical Gravitational Lensing Experiment. Additional Planetary and Low-Luminosity Object Transits from the OGLE 2001 and 2002 Observational Campaigns". Acta Astronomica 53: 133. (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" (abstract). Astronomy and Astrophysics 458: 997-1005. doi:10.1051/0004-6361:20065683. (web Preprint)
  3. ^ a b c 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 Gillon et al. (2007). "The transiting planet OGLE-TR-132b revisited with new spectroscopy and deconvolution photometry" (abstract). Astronomy and Astrophysics 466: 743-748. doi:10.1051/0004-6361:20066367. (web Preprint)

[edit] External links

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