WASP-69

WASP-69 / Wouri
Observation data
Epoch J2000      Equinox ICRS
Constellation Aquarius
Right ascension 21h 00m 06.19682s
Declination −05° 05′ 40.0349″
Apparent magnitude (V) 9.87±0.03
Characteristics
Evolutionary stage main sequence
Spectral type K5V
Astrometry
Radial velocity (Rv)−9.83±0.13 km/s
Proper motion (μ) RA: 33.778 mas/yr
Dec.: −93.581 mas/yr
Parallax (π)19.8858±0.0170 mas
Distance164.0 ± 0.1 ly
(50.29 ± 0.04 pc)
Details
Mass0.826±0.029 M☉
Radius0.813 R☉
Luminosity0.34 L☉
Surface gravity (log g)4.59±0.02 cgs
Temperature4,782±15 K
Metallicity [Fe/H]0.10±0.01 dex
Rotation23.07 d
Rotational velocity (v sin i)1.27±0.22 km/s
Age2 Gyr
Other designations
Wouri, BD−05 5432, TOI-5823, TIC 248853232, WASP-69, TYC 5200-1560-1, GSC 05200-01560, 2MASS J21000618-0505398
Database references
SIMBADdata
Exoplanet Archivedata

WASP-69, also named Wouri, is a K-type main-sequence star 164 light-years (50 parsecs) away from Earth in the constellation Aquarius. Its surface temperature is 4782±15 K. WASP-69 is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.10±0.01, and is much younger than the Sun at 2 billion years. The data regarding starspot activity of WASP-69 are inconclusive, but spot coverage of the photosphere may be very high.

Multiplicity surveys did not detect any stellar companions to WASP-69 as of 2020.

Nomenclature

The designation WASP-69 indicates that this was the 69th star found to have a planet by the Wide Angle Search for Planets.

In August 2022, this planetary system was included among 20 systems to be named by the third NameExoWorlds project. The approved names, proposed by a team from Cameroon, were announced in June 2023. WASP-69 is named Wouri and its planet is named Makombé, after the Wouri and Makombé rivers in Cameroon.

Planetary system

In 2013, one planet, named WASP-69b, was discovered on a tight, circular orbit. Its equilibrium temperature is 886 K, but the measured terminator temperature is significantly higher by at least 200 K. The planet is losing mass at a moderate rate of 0.5 M🜨 per billion years, producing a tail detected in 2024 and measured to be at least 7 times its own radius.

The planetary atmosphere is extremely hazy and contains a partial cloud deck with cloud tops rising to a pressure of 100 Pa. Its composition is mostly hydrogen and helium, and sodium was also detected in low concentration. The sodium may originate from volcanic moons, not from the planet itself.

By 2021, the presence of hazes in atmosphere of WASP-69b was confirmed, along with a solar or super-solar water abundance.

The WASP-69 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination
(°)		 Radius
b / Makombé 0.260±0.017 MJ 0.04525±0.00053 3.8681382±0.0000017 0 86.71±0.20 0.945+0.007
−0.017 RJ

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. 1 2 3 4 5 6 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. 1 2 3 4 5 6 7 8 Anderson, D. R.; Collier Cameron, A.; Delrez, L.; Doyle, A. P.; Faedi, F.; Fumel, A.; Gillon, M.; Gómez Maqueo Chew, Y.; Hellier, C.; Jehin, E.; Lendl, M.; Maxted, P. F. L.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Skillen, I.; Smalley, B.; Smith, A. M. S.; Southworth, J.; Triaud, A. H. M. J.; Turner, O. D.; Udry, S.; West, R. G. (2014). "Three newly discovered sub-Jupiter-mass planets: WASP-69b and WASP-84b transit active K dwarfs and WASP-70Ab transits the evolved primary of a G4+K3 binary". Monthly Notices of the Royal Astronomical Society. 445 (2): 1114–1129. arXiv:1310.5654. doi:10.1093/mnras/stu1737. S2CID 54750890.
  4. ↑ France, Kevin; Arulanantham, Nicole; Fossati, Luca; Lanza, Antonino F.; Loyd, R. O. Parke; Redfield, Seth; Schneider, P. Christian (2018), "Far-ultraviolet Activity Levels of F, G, K, and M Dwarf Exoplanet Host Stars", The Astrophysical Journal Supplement Series, 239 (1): 16, arXiv:1809.07342, Bibcode:2018ApJS..239...16F, doi:10.3847/1538-4365/aae1a3, S2CID 119368148
  5. ↑ Yu, Jie; Khanna, Shourya; Themessl, Nathalie; Hekker, Saskia; Dréau, Guillaume; Gizon, Laurent; Bi, Shaolan (2023). "Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE". The Astrophysical Journal Supplement Series. 264 (2): 41. arXiv:2206.00046. Bibcode:2023ApJS..264...41Y. doi:10.3847/1538-4365/acabc8.
  6. 1 2 3 4 5 Gill, S.; Maxted, P. F. L.; Smalley, B. (2018). "The atmospheric parameters of FGK stars using wavelet analysis of CORALIE spectra". Astronomy & Astrophysics. 612: A111. arXiv:1801.06106. Bibcode:2018A&A...612A.111G. doi:10.1051/0004-6361/201731954. S2CID 119331772.
  7. ↑ "BD-05 5432". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-01-08.
  8. 1 2 Andrews, Robin George (12 January 2024). "This Distant Planet Has a 350,000-Mile-Long Comet-Like Tail - The stream of helium trailing WASP-69b, a "Hot Jupiter," allows astronomers to study how planets lose their atmospheres". The New York Times. Retrieved 12 January 2024.{{cite news}}: CS1 maint: deprecated archival service (link)
  9. 1 2 3 4 Murgas, F.; Chen, G.; Nortmann, L.; Pallé, E.; Nowak, G. (2020). "The GTC exoplanet transit spectroscopy survey XI. Possible detection of Rayleigh scattering in the atmosphere of the Saturn-mass planet WASP-69b". Astronomy & Astrophysics. A158: 641. arXiv:2007.02741. Bibcode:2020A&A...641A.158M. doi:10.1051/0004-6361/202038161. S2CID 220363912.
  10. ↑ Bohn, A. J.; Southworth, J.; Ginski, C.; Kenworthy, M. A.; Maxted, P. F. L.; Evans, D. F. (2020), "A multiplicity study of transiting exoplanet host stars. I. High-contrast imaging with VLT/SPHERE", Astronomy & Astrophysics, 635: A73, arXiv:2001.08224, Bibcode:2020A&A...635A..73B, doi:10.1051/0004-6361/201937127, S2CID 210861118
  11. ↑ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
  12. ↑ "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
  13. 1 2 Wang, Lile; Dai, Fei (2021). "Metastable Helium Absorptions with 3D Hydrodynamics and Self-consistent Photochemistry. I. WASP-69b, Dimensionality, X-Ray and UV Flux Level, Spectral Types, and Flares". The Astrophysical Journal. 914 (2): 98. arXiv:2101.00042. Bibcode:2021ApJ...914...98W. doi:10.3847/1538-4357/abf1ee. S2CID 230433986.
  14. ↑ Tyler, Dakotah; Petigura, Erik A.; Oklopčić, Antonija; David, Trevor J. (9 January 2024). "WASP-69b's Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp". The Astrophysical Journal. 960 (2): 123. arXiv:2312.02381. Bibcode:2024ApJ...960..123T. doi:10.3847/1538-4357/ad11d0.
  15. ↑ Casasayas-Barris, N.; Palle, E.; Nowak, G.; Yan, F.; Nortmann, L.; Murgas, F. (2017), "Detection of sodium in the atmosphere of WASP-69b", Astronomy & Astrophysics, 608: A135, arXiv:1710.06479, Bibcode:2017A&A...608A.135C, doi:10.1051/0004-6361/201731956, S2CID 67777582
  16. ↑ Oza, Apurva V.; Johnson, Robert E.; Lellouch, Emmanuel; Schmidt, Carl; Schneider, Nick; Huang, Chenliang; Gamborino, Diana; Gebek, Andrea; Wyttenbach, Aurelien; Demory, Brice-Olivier; Mordasini, Christoph; Saxena, Prabal; Dubois, David; Moullet, Arielle; Thomas, Nicolas (2019), "Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets", The Astrophysical Journal, 885 (2): 168, arXiv:1908.10732, Bibcode:2019ApJ...885..168O, doi:10.3847/1538-4357/ab40cc, S2CID 201651224
  17. ↑ Khalafinejad, S.; et al. (2021), "Probing the atmosphere of WASP-69 b with low- and high-resolution transmission spectroscopy", Astronomy & Astrophysics, 656: A142, arXiv:2109.06335, Bibcode:2021A&A...656A.142K, doi:10.1051/0004-6361/202141191, S2CID 237503489