WASP-74
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Aquila[1] |
| Right ascension | 20h 18m 09.32s[2] |
| Declination | −01° 04′ 33.6″[2] |
| Apparent magnitude (V) | 9.75[2] |
| Characteristics | |
| Evolutionary stage | subgiant[3] |
| Spectral type | F9[4] |
| B−V color index | 0.64[2] |
| Astrometry | |
| Radial velocity (Rv) | −15.32±0.27[2] km/s |
| Proper motion (μ) | RA: +1.350±0.082[2] mas/yr Dec.: −64.604±0.060[2] mas/yr |
| Parallax (π) | 6.6734±0.0508 mas[2] |
| Distance | 489 ± 4 ly (150 ± 1 pc) |
| Details | |
| Mass | 1.236±0.026[5] M☉ |
| Radius | 1.444±0.044[5] R☉ |
| Luminosity | 2.65[6] L☉ |
| Surface gravity (log g) | 4.32[6] cgs |
| Temperature | 5,883±57[5] K |
| Metallicity [Fe/H] | 0.38±0.03[5] dex |
| Rotational velocity (v sin i) | 5.85±0.50[5] km/s |
| Age | 3.49±0.65[5] Gyr |
| Other designations | |
| BD−01°3943, TIC 244089109, TYC 5162-1142-1, 2MASS J20180931-0104324, Gaia DR2 4224062406762625152 | |
| Database references | |
| SIMBAD | data |
WASP-74 is a star in the constellation of Aquila, located approximately 487 light-years (149 parsecs) from the Sun.[2] At least one exoplanet is known to orbit the star.
Stellar characteristics
[edit]WASP-74 is a yellow-white subgiant of spectral type F9. Its apparent magnitude is 9.75, making it invisible to the naked eye. Based on spectroscopic analysis with the HARPS-N spectrograph and Bayesian modelling using PARSEC isochrones, the star has a mass of 1.236 ± 0.026 solar masses, a radius of 1.444±0.044 solar radii, and an effective temperature of 5,883±57 K. Its metallicity ([Fe/H]) is +0.38±0.03, indicating it is notably more metal-rich than the Sun. Stellar models give an age of 3.49±0.65 billion years, and the star's projected rotational velocity is 5.85±0.50 km/s.[5]
The star's proper motion is 1.350±0.082 mas/yr in right ascension and −64.604±0.060 mas/yr in declination, with a radial velocity of −15.32±0.27 km/s.[2]
Planetary system
[edit]In 2015, one exoplanet was announced orbiting WASP-74, designated WASP-74 b, discovered by the SuperWASP survey using the transit method.[4] It is a hot Jupiter with a mass of 0.72 Jupiter masses and a radius of 1.312 Jupiter radii, completing one orbit every 2.13775138 days at a distance of 0.0334 AU from its host star, with an equilibrium temperature of approximately 1,865 K. The planet's orbit is circular and well-aligned with the stellar equator, with a measured sky-projected spin-orbit angle of 0.77±0.99 degrees.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| b | 0.72 MJ | 0.0334 | 2.13775138 | 0 | — | 1.312 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 8 9 10 "WASP-74". NASA Exoplanet Archive. Retrieved 2026-04-01.
- ↑ 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.
- 1 2 Hellier, C.; et al. (2015). "Three WASP-South Transiting Exoplanets: WASP-74b, WASP-83b, and WASP-89b". The Astronomical Journal. 150 (1): 18. arXiv:1410.6358. Bibcode:2015AJ....150...18H. doi:10.1088/0004-6256/150/1/18.
- 1 2 3 4 5 6 7 8 Luque, R.; et al. (2020). "Obliquity measurement and atmospheric characterisation of the WASP-74 planetary system". Astronomy & Astrophysics. 642: A50. arXiv:2007.11851. Bibcode:2020A&A...642A..50L. doi:10.1051/0004-6361/202038703.
- 1 2 De Laverny, Patrick; Ligi, Roxanne; Crida, Aurélien; Recio-Blanco, Alejandra; Palicio, Pedro A. (2025). "The Gaia spectroscopic catalogue of exoplanets and host stars". Astronomy and Astrophysics. 699: A100. arXiv:2505.22205. Bibcode:2025A&A...699A.100D. doi:10.1051/0004-6361/202554739.
