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WASP-66

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, which is much too faint to be seen with the unaided eye and is located at a distance of 1,630 light-years.

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WASP-66
Observation data
Epoch J2000      Equinox J2000
Constellation Antlia1
Right ascension 10h 32m 53.993s2
Declination −34° 59′ 23.46″2
Apparent magnitude (V) 11.603
Characteristics
Evolutionary stage main sequence2
Spectral type F44
Astrometry
Radial velocity (Rv)−9.79±0.962 km/s
Proper motion (μ) RA: 11.452 mas/yr2
Dec.: −13.476 mas/yr2
Parallax (π)1.9962±0.0313 mas2
Distance1,630 ± 30 ly
(501 ± 8 pc)
Details5
Mass1.30±0.07 M☉
Radius1.75±0.09 R☉
Luminosity4.36 L☉
Surface gravity (log g)5.007 cgs
Temperature6,600±150 K
Metallicity [Fe/H]0.057 dex
Rotational velocity (v sin i)13.4±0.9 km/s
Age3.7+0.7
−1.2 Gyr
Other designations
TOI-661, TIC 53735810, WASP-66, TYC 7193-1804-1, 2MASS J10325399-34592348
Database references
SIMBADdata
Exoplanet Archivedata

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 Sun at 3.7+0.7
−1.2 billion years, and may be either metal-poor5 or similar to Sun7 in 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

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

The WASP-66 planetary system5
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

References

  1. 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.
  2. 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.
  3. 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.
  4. 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.
  5. 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.
  6. 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.
  7. 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.
  8. "WASP-66". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 21 January 2017.
  9. 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.
  10. 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.