 Size comparison of COROT-23b with Jupiter. | |
| Discovery | |
|---|---|
| Discovery site | Earth's orbit |
| Transit method | |
| Orbital characteristics | |
| 0.0281 ± 0.0005[1][2] | |
| Eccentricity | 0 (assumed)[1] |
| 1.7429964 ± 0.0000017[1] | |
| Inclination | 87.84 ± 0.10[1] |
| Star | COROT-23 |
| Physical characteristics | |
| Mass | 3.31 ± 0.16[1] |
Mean density | 1310 ± 40[1] |
COROT-23b is an extrasolar planet detected by the French-led COROT mission, which orbits the star COROT-23 at a distance of 1960 light years from Earth towards the constellation Aquila. After its discovery via the transit method, its mass was confirmed via the radial velocity method.
Characteristics
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The planet is a large hot Jupiter, about 1.43 times the radius of Jupiter and approximately 3.3 times as massive. Its huge size is due to the intense heating from its parent star, which causes the outer layers of its atmosphere to bloat. The extremely large radius of the planet indicates that COROT-2b is really hot, estimated to be around 1500 K, even hotter than would be expected given its location close to its parent star. This fact may be a sign of tidal heating due to interactions with another planet.[5] At Jupiter-like distances its radius would roughly be the same as Jupiter.[6]
COROT-2b orbits its star approximately once every 1.7 days, and orbits the star in a prograde direction close to the star's equator.[3] Its parent star is a G-type star, a bit cooler than the Sun but more active. It is located about 800 light-years from Earth.
It takes 125 minutes to transit its star.[7]
As of August 2008, the COROT-2b spin-orbit angle (that is, the angle between the equator of the star and the plane of the planet orbit) was calculated by Bouchy et al. by mean of the Rossiter-McLaughlin effect[8] with a value of +7.2 ± 4.5 degrees.[9]
References
edit- ^ a b c d e f g h i j k
Rouan, D., et al (2012). "Transiting exoplanets from the CoRoT space mission XIX. CoRoT-23b: a dense hot Jupiter on an eccentric orbit". Astronomy and Astrophysics. 537: A54. doi:10.1051/0004-6361/201117916.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ The paper gives the semimajor axis as 6.70 ± 0.03 times the radius of the star, which is estimated at 0.902 ± 0.018 solar radii.
- ^ a b
Bouchy, F.; et al. (2008). "Transiting exoplanets from the CoRoT space mission. III. The spectroscopic transit of CoRoT-Exo-2b with SOPHIE and HARPS". Astronomy and Astrophysics. 482 (3): L25–L28. arXiv:0803.3209. Bibcode:2008A&A...482L..25B. doi:10.1051/0004-6361:200809433.
{{cite journal}}: CS1 maint: date and year (link) - ^ Calculated using Newtonian gravity:
- ^ "CoRoT-exo-2 c?". Retrieved 21 December 2007.
- ^ Gibor Basri; Brown (20 August 2006). "Planetesimals to Brown Dwarfs: What is a Planet?". Ann.Rev.Earth Planet.Sci. 34 (2006) 193-216. 34: 193–216. arXiv:astro-ph/0608417. Bibcode:2006AREPS..34..193B. doi:10.1146/annurev.earth.34.031405.125058.
- ^ "Predicted Transit Epochs: CoRoTExo2 b". TransitSearch (Oklo Corporation). Retrieved 15 July 2009.
{{cite web}}: External link in|publisher= - ^ Joshua N. Winn (2008). "Measuring accurate transit parameters". Proceedings of the International Astronomical Union. 4: 99–109. arXiv:0807.4929. doi:10.1017/S174392130802629X.
- ^ Bouchy; Queloz, D.; Deleuil, M.; Loeillet, B.; Hatzes, A. P.; Aigrain, S.; Alonso, R.; Auvergne, M.; Baglin, A.; et al. (2008). "Transiting exoplanets from the CoRoT space mission. III. The spectroscopic transit of CoRoT-Exo-2b with SOPHIE and HARPS". Astronomy and Astrophysics. 482 (3): L25. arXiv:0803.3209. Bibcode:2008A&A...482L..25B. doi:10.1051/0004-6361:200809433.
{{cite journal}}: Explicit use of et al. in:|author=(help)
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