OGLE-TR-111b

In the following article we will analyze OGLE-TR-111b in depth, a topic that has generated great interest and debate in recent years. Since its emergence, OGLE-TR-111b has captured the attention of experts and fans alike, generating a wide range of opinions and theories. Throughout this article, we will explore the different facets of OGLE-TR-111b, from its impact on today's society to its relevance in the historical context. Additionally, we will examine the future implications of OGLE-TR-111b and the role it could play in our daily lives. This analysis seeks to offer a comprehensive perspective on OGLE-TR-111b, with the aim of enriching knowledge and understanding of this very relevant topic.
OGLE-TR-111b
Size comparison of OGLE-TR-111b with Jupiter
Discovery
Discovered byUdalski et al.[1]
Discovery site Poland
Discovery date2002[1]
Transit and Doppler
Orbital characteristics
0.047 ± 0.001 AU (7,030,000 ± 150,000 km)
Eccentricity0
4.01610 d
Inclination88.1
2,452,330.44867
StarOGLE-TR-111
Physical characteristics
1.067 RJ
Mass0.53 ± 0.11 MJ
Mean density
0.70 g/cm3
12.5 m/s2 (1.27 g0)

OGLE-TR-111b is an extrasolar planet approximately 5,000 light-years away in the constellation of Carina (the Keel). The planet is currently the only confirmed planet orbiting the star OGLE-TR-111 (though a possible second planet is plausible).

In 2002 the Optical Gravitational Lensing Experiment (OGLE) survey detected that the light from the star periodically dimmed very slightly every 4 days, indicating a planet-sized body transiting the star. But since the mass of the object had not been measured, it was not clear that it was a true planet, low-mass red dwarf or something else.[1] In 2004 radial velocity measurements showed unambiguously that the transiting body is indeed a planet.[2]

The planet is probably very similar to the other hot Jupiters orbiting nearby stars. Its mass is about half that of Jupiter and it orbits the star at a distance less than 1/20th that of Earth from the Sun.

OGLE-TR-111b has similar mass and orbital distance as the first transiting planet, HD 209458 b (Osiris). But unlike it, the planet has a radius comparable to Jupiter which is typical to other transiting planets detected by OGLE. However, those other planets tend to be more massive and orbit even closer than typical hot Jupiters. Therefore, this planet is an important "missing link" between the different types of transiting planets.[3]

See also

References

  1. ^ a b c Udalski, A.; 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 (4): 317–359. arXiv:astro-ph/0301210. Bibcode:2002AcA....52..317U.
  2. ^ Pont, F.; et al. (2004). "The "missing link" : A 4-day period transiting exoplanet around OGLE-TR-111". Astronomy and Astrophysics. 426: L15 – L18. arXiv:astro-ph/0408499. Bibcode:2004A&A...426L..15P. doi:10.1051/0004-6361:200400066. S2CID 16553970.
  3. ^ Minniti, Dante; et al. (2007). "Millimagnitude Photometry for Transiting Extrasolar Planetary Candidates. III. Accurate Radius and Period for OGLE-TR-111-b". The Astrophysical Journal. 660 (1): 858–862. arXiv:astro-ph/0701356. Bibcode:2007ApJ...660..858M. doi:10.1086/512722. S2CID 16876570.

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