CoRoT-6 is a magnitude 13.9 star located in the Ophiuchus constellation.[6]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Ophiuchus |
| Right ascension | 18h 44m 17.4079s[1] |
| Declination | +6° 39′ 47.513″[1] |
| Apparent magnitude (V) | 13.9[2] |
| Characteristics | |
| Spectral type | F5V[3] |
| Astrometry | |
| Proper motion (μ) | RA: 5.438±0.017[1] mas/yr Dec.: 1.889±0.016[1] mas/yr |
| Parallax (π) | 1.5641 ± 0.0163 mas[1] |
| Distance | 2,090 ± 20 ly (639 ± 7 pc) |
| Details | |
| Mass | 1.1[2] M☉ |
| Radius | 1.02[2] R☉ |
| Luminosity | 1.4[1] L☉ |
| Surface gravity (log g) | 428[1] cgs |
| Temperature | 5,922[1] K |
| Metallicity [Fe/H] | −0.20[4] dex |
| Rotational velocity (v sin i) | 7.5[5] km/s |
| Age | 4.9[1] Gyr |
| Other designations | |
CoRoT-Exo-6[2] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
Location and properties
editThe star has a radius of about 102% of the Sun and a mass of about 110% of the Sun.[2] It is a main sequence F type star a little larger and hotter than the Sun.
Planetary system
editThe star is orbited by one known extrasolar planet identified as CoRoT-6b. The discovery was made by the CoRoT program using the transit method.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 2.96 MJ | 0.0855 | 8.887 | < 0.1 | — | 1.166 RJ |
References
edit- ^ a b c d e f g h i Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f H. Rauer, M. Fridlund (2009). "CoRoT's exoplanet harvest" (PDF). First CoRoT International Symposium. Archived from the original (PDF) on 2011-07-20. Retrieved 2009-04-19.
- ^ Ehrenreich, D.; Désert, J.-M. (2011). "Mass-loss rates for transiting exoplanets". Astronomy & Astrophysics. 529: A136. arXiv:1103.0011. Bibcode:2011A&A...529A.136E. doi:10.1051/0004-6361/201016356. S2CID 119302960.
- ^ Chen, Di-Chang; Xie, Ji-Wei; Zhou, Ji-Lin; Dong, Subo; Liu, Chao; Wang, Hai-Feng; Xiang, Mao-Sheng; Huang, Yang; Luo, Ali; Zheng, Zheng (2021). "Planets Across Space and Time (PAST). I. Characterizing the Memberships of Galactic Components and Stellar Ages: Revisiting the Kinematic Methods and Applying to Planet Host Stars". The Astrophysical Journal. 909 (2): 115. arXiv:2102.09424. Bibcode:2021ApJ...909..115C. doi:10.3847/1538-4357/abd5be. S2CID 231951508.
- ^ Damiani, C.; Lanza, A. F. (2015). "Evolution of angular-momentum-losing exoplanetary systems. Revisiting Darwin stability". Astronomy and Astrophysics. 574. arXiv:1411.3802. Bibcode:2015A&A...574A..39D. doi:10.1051/0004-6361/201424318. S2CID 54727372.
- ^ a b Fridlund, M.; et al. (2010). "Transiting exoplanets from the CoRoT space mission. IX. CoRoT-6b: a transiting 'hot Jupiter' planet in an 8.9d orbit around a low-metallicity star". Astronomy and Astrophysics. 512. A14. arXiv:1001.1426v1. Bibcode:2010A&A...512A..14F. doi:10.1051/0004-6361/200913767. S2CID 54014374.
 | This main-sequence-star-related article is a stub. You can help Wikipedia by expanding it. |