WASP-66
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Antlia[1] |
| Right ascension | 10h 32m 53.993s[2] |
| Declination | −34° 59′ 23.46″[2] |
| Apparent magnitude (V) | 11.60[3] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | F4[4] |
| Astrometry | |
| Radial velocity (Rv) | −9.79±0.96[2] km/s |
| Proper motion (μ) | RA: 11.452 mas/yr[2] Dec.: −13.476 mas/yr[2] |
| Parallax (π) | 1.9962±0.0313 mas[2] |
| Distance | 1,630 ± 30 ly (501 ± 8 pc) |
| Details[5] | |
| Mass | 1.30±0.07 M☉ |
| Radius | 1.75±0.09 R☉ |
| Luminosity | 4.3[6] L☉ |
| Surface gravity (log g) | 5.00[7] cgs |
| Temperature | 6,600±150 K |
| Metallicity [Fe/H] | 0.05[7] dex |
| Rotational velocity (v sin i) | 13.4±0.9 km/s |
| Age | 3.7+0.7 −1.2 Gyr |
| Other designations | |
| TOI-661, TIC 53735810, WASP-66, TYC 7193-1804-1, 2MASS J10325399-3459234[8] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
WASP-66, also known as TYC 7193-1804-1, is an F-type star in the constellation Antlia. It has an apparent magnitude of 11.6,[8] which is much too faint to be seen with the unaided eye and is located at a distance of 1,630 light-years.
WASP-66 has a classification of F4, which states that it is an ordinary F-type main sequence star that is fusing hydrogen at its core. At present it has 130% the mass of the Sun and 175 the radius of the Sun.[5] It has an effective temperature of 6,600 K,[5] which gives it a yellowish-white hue. The star is younger than the Sun at, 3.7+0.7
−1.2 billion years, and may be either metal-poor[5] or similar to Sun[7] in its concentration of heavy elements. Currently it is spinning moderately with a projected rotational velocity of 13.4 km/s.[5]
According to a survey published in 2017, WASP-66 has one suspected companion - a red dwarf star with an effective temperature of 3,330±150 K and a projected separation of 6,800±700 AU.[9]
Planetary system
[edit]In 2012, a superjovian planet around WASP-66 was discovered. WASP-66b has a mass that is about 2.3 times that of Jupiter. It takes just over 4 days to complete an orbit around its star, making it a typical hot Jupiter. The planet was discovered by the transit method – this is when a planet passes in front of a star, temporarily blocking some of the star's light.[4]
The planetary orbit is well aligned with the equatorial plane of the star, the misalignment angle being equal to −4±22°.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| b | 2.37±0.14 MJ | 0.05461+0.00099 −0.00096 |
4.0860520±0.000007 | <0.046 | 85.9±0.9 | 1.09+0.25 −0.19 RJ |
References
[edit]- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- 1 2 3 4 5 6 7 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.
- ↑ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
- 1 2 Hellier, Coel; et al. (2012). "Seven transiting hot Jupiters from WASP-South, Euler and TRAPPIST: WASP-47b, WASP-55b, WASP-61b, WASP-62b, WASP-63b, WASP-66b and WASP-67b". Monthly Notices of the Royal Astronomical Society. 426 (1): 739–750. arXiv:1204.5095. Bibcode:2012MNRAS.426..739H. doi:10.1111/j.1365-2966.2012.21780.x. S2CID 54713354.
- 1 2 3 4 5 6 Bonomo, A. S.; et al. (2017). "The GAPS Programme with HARPS-N at TNG". Astronomy & Astrophysics. 602: A107. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882. S2CID 118923163.
- ↑ Johns, Daniel; et al. (November 2018). "Revised Exoplanet Radii and Habitability Using Gaia Data Release 2". The Astrophysical Journal Supplement Series. 239 (1): 14. arXiv:1808.04533. Bibcode:2018ApJS..239...14J. doi:10.3847/1538-4365/aae5fb. 14.
- 1 2 3 Delgado Mena, E. (2015). "Li abundances in F stars: planets, rotation, and Galactic evolution". Astronomy & Astrophysics. 576: A69. arXiv:1412.4618. Bibcode:2015A&A...576A..69D. doi:10.1051/0004-6361/201425433. S2CID 56051637.
- 1 2 "WASP-66". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 21 January 2017.
- ↑ Evans, D. F.; et al. (2017). "High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)". Astronomy & Astrophysics. 610: A20. arXiv:1709.07476. Bibcode:2018A&A...610A..20E. doi:10.1051/0004-6361/201731855. S2CID 53400492.
- ↑ Addison, B. C.; Tinney, C. G.; Wright, D. J.; Bayliss, D. (2016). "SPIN–ORBIT ALIGNMENT FOR THREE TRANSITING HOT JUPITERS: WASP-103b, WASP-87b, and WASP-66b". The Astrophysical Journal. 823 (1): 29. arXiv:1603.05754. Bibcode:2016ApJ...823...29A. doi:10.3847/0004-637X/823/1/29. S2CID 118686465.
