CoRoT-2

CoRoT-2 is a yellow dwarf main sequence star a little cooler than the Sun. This star is located approximately 700 light-years away in the constellation of Aquila. The apparent magnitude of this star is 12, which means it is not visible to the naked eye but can be seen with a medium-sized amateur telescope on a clear dark night.[2]

CoRoT-2

CoRoT-2 is a G7V class star somewhat less massive than the Sun (G2V)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Aquila
Right ascension  19h 27m 06.4945s[1]
Declination +01° 23′ 01.3576″[1]
Apparent magnitude (V) 12.57[2]
Characteristics
Spectral type G7V[3]
K0V (SIMBAD)[2]
Apparent magnitude (V) ~12.577
Apparent magnitude (I) 11.49 ±0.03
Apparent magnitude (J) 10.5783 ±0.028
Apparent magnitude (H) 10.44 ±0.04
Apparent magnitude (K) 10.31 ±0.03
Astrometry
Proper motion (μ) RA: −3.409±0.084[1] mas/yr
Dec.: −10.936±0.074[1] mas/yr
Parallax (π)4.6608 ± 0.0536[1] mas
Distance700 ± 8 ly
(215 ± 2 pc)
Details
Mass0.97 ±0.06 M☉
Radius0.902 ±0.018 R☉
Temperature5625 ±120 K
Metallicity0 ±0.1
Age? years
Other designations
GSC 00465-01282, CoRoT-Exo-2, GSC2 N023200075, UCAC2 32263596, CoRoT 101206560, DENIS-P J192706.4+012301, 2MASS J19270649+0123013, USNO-B1.0 0913-00447544[2]
Database references
SIMBADdata
Extrasolar Planets
Encyclopaedia		data

It has a true physical companion, 2MASS J19270636+0122577, with a spectral type of K9, as earlier hypothesized by Alonso et al. (2008), making CoRoT-2 a wide binary system with at least one planet.[4]

Planetary system

This star is home to exoplanet CoRoT-2b discovered by the CoRoT Mission spacecraft using the transit method.[3] CoRoT-2b (formerly known as CoRoT-Exo-2b[5]) is the second extrasolar planet to be detected by the French-led CoRoT mission, and orbits the star CoRoT-2 at a distance of 930 light years from Earth towards the constellation Aquila. Its discovery was announced on 20 December 2007.[6] After its discovery via the transit method, its mass was confirmed via the radial velocity method.

The radial velocity trend of CoRoT-2, caused by the presence of CoRoT-2 b.

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.[7] At Jupiter-like distances its radius would roughly be the same as Jupiter.[8] The complete phase curve of this planet has been observed.[9]

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.[10] 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.[11]

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 means of the Rossiter–McLaughlin effect[12] with a value of +7.2 ± 4.5 degrees.[10]

The CoRoT-2 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 3.31 ±0.16 MJ 0.0281 ±0.0009 1.7429964 ±1.7e-06 0 — —
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See also
  • List of extrasolar planets

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. "GSC 00465-01282". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-04-27.
  3. Alonso, R.; et al. (2008). "Transiting exoplanets from the CoRoT space mission. II. CoRoT-Exo-2b: a transiting planet around an active G star". Astronomy and Astrophysics. 482 (3): L21–L24. arXiv:0803.3207. Bibcode:2008A&A...482L..21A. doi:10.1051/0004-6361:200809431.
  4. S. Czesla; S. Schröter; U. Wolter; C. von Essen; K. F. Huber; J. H. M. M. Schmitt; D. E. Reichart; J. P. Moore (March 2012). "The extended chromosphere of CoRoT-2A: Discovery and analysis of the chromospheric Rossiter-McLaughlin effect". Astronomy and Astrophysics. 539: A150. Bibcode:2012A&A...539A.150C. doi:10.1051/0004-6361/201118042.
  5. Schneider, J. (10 March 2009). "Change in CoRoT planets names". Exoplanets (Mailing list). Archived from the original on 18 January 2010. Retrieved 2009-03-19.
  6. "COROT surprises a year after launch". Retrieved 2007-12-21.
  7. "CoRoT-exo-2 c?". Retrieved 2007-12-21.
  8. Gibor Basri; Brown (20 August 2006). "Planetesimals to Brown Dwarfs: What is a Planet?". Annu. Rev. Earth Planet. Sci. 34: 193–216. arXiv:astro-ph/0608417. Bibcode:2006AREPS..34..193B. doi:10.1146/annurev.earth.34.031405.125058.
  9. Cowan, Nicolas; Deming, Drake; Gillon, Michael; Knutson, Heather; Madhusudhan, Nikku; Rauscher, Emily (2011). "Phase Variations, Transits and Eclipses of the Misfit CoRoT-2b". Spitzer Proposal: 80044. Bibcode:2011sptz.prop80044C.CS1 maint: uses authors parameter (link)
  10. Bouchy, F.; Queloz, D.; Deleuil, M.; Loeillet, B.; Hatzes, A. P.; Aigrain, S.; Alonso, R.; Auvergne, M.; Baglin, A.; Barge, P.; Benz, W.; Bordé, P.; Deeg, H. J.; De La Reza, R.; Dvorak, R.; Erikson, A.; Fridlund, M.; Gondoin, P.; Guillot, T.; Hébrard, G.; Jorda, L.; Lammer, H.; Léger, A.; Llebaria, A.; Magain, P.; Mayor, M.; Moutou, C.; Ollivier, M.; Pätzold, M.; et al. (2008). "Transiting exoplanets from the CoRoT space mission". Astronomy and Astrophysics. 482 (3): L25. arXiv:0803.3209. Bibcode:2008A&A...482L..25B. doi:10.1051/0004-6361:200809433.
  11. "Predicted Transit Epochs: CoRoTExo2 b". TransitSearch (Oklo Corporation). Retrieved 2009-07-15.
  12. Joshua N. Winn (2008). "Measuring accurate transit parameters". Proceedings of the International Astronomical Union. 4: 99–109. arXiv:0807.4929. Bibcode:2009IAUS..253...99W. doi:10.1017/S174392130802629X.

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