WASP-94

WASP-94
Observation data
Epoch J2000      Equinox ICRS
Constellation Microscopium[1]
A
Right ascension 20h 55m 07.94435s[2]
Declination −34° 08′ 08.0075″[2]
Apparent magnitude (V) 10.1[3]
B
Right ascension 20h 55m 09.15767s[4]
Declination −34° 08′ 07.9138″[4]
Apparent magnitude (V) 10.5[3]
Characteristics
A
Evolutionary stage main sequence[2]
Spectral type F8[3]
B
Evolutionary stage subgiant[4]
Spectral type F9[3]
Astrometry
A
Radial velocity (Rv)−8.36±0.19[2] km/s
Proper motion (μ) RA: +26.500 mas/yr[2]
Dec.: −44.971 mas/yr[2]
Parallax (π)4.7498±0.0242 mas[2]
Distance687 ± 3 ly
(211 ± 1 pc)
B
Radial velocity (Rv)−8.30±0.20[4] km/s
Proper motion (μ) RA: +26.191 mas/yr[4]
Dec.: −44.702 mas/yr[4]
Parallax (π)4.7208±0.0165 mas[4]
Distance691 ± 2 ly
(211.8 ± 0.7 pc)
Details
A
Mass1.45±0.09[3] M☉
Radius1.62+0.05
−0.04[3] R☉
Luminosity3.2[5] L☉
Surface gravity (log g)4.21±0.011[6] cgs
Temperature6194±5[6] K
Metallicity [Fe/H]+0.320±0.004[6] dex
Rotation19.5 d[3]
Rotational velocity (v sin i)4.2±0.5[3] km/s
Age2.3–2.8[6] Gyr
B
Mass1.24±0.09[3] M☉
Radius1.35±0.12[3] R☉
Luminosity2.2[7] L☉
Surface gravity (log g)4.30±0.015[6] cgs
Temperature6112±6[6] K
Metallicity [Fe/H]+0.305±0.005[6] dex
Rotation>45.5 d[3]
Rotational velocity (v sin i)<1.5[3] km/s
Age2.3–2.8[6] Gyr
Other designations
CD−34 14724, WASP-94, HJ 5234
A: TOI-107, TIC 92352620, TYC 7466-1400-1, 2MASS J20550794-3408079[8]
B: TIC 92352621, 2MASS J20550915-3408078[9]
Database references
SIMBADA
B
Exoplanet Archivedata

WASP-94 is a binary star system located about 690 light-years (210 parsecs) away in the constellation Microscopium. It consists of two F-type stars separated by 15″, corresponding to a projected separation of 2700 au. Both stars are known to host exoplanets.[3]

The binary system was first observed by John Herschel in 1834 and catalogued as HJ 5234. The designation WASP-94 comes from the Wide Angle Search for Planets, and has been used since the system was found to host planets in 2014.[3] While the two stars have similar spectral types, they differ in elemental abundance – WASP-94A has fewer volatile elements and more refractory elements than WASP-94B.[6]

Planetary system

The two stars host a single known planet each. Both are hot Jupiters, gas giant planets completing orbits around their stars in just a few days.[3]

Diagram of the WASP-94 system

WASP-94Ab transits its host star, and it has also been detected by the radial velocity method.[3] As a result, both its size and mass are known, which show that it is a low-density planet with a highly inflated radius. It has an equilibrium temperature of 1508±75 K.[10] Its orbit is retrograde and misaligned with the rotation of its host star.[11] The atmosphere of WASP-94Ab appears to be relatively free of clouds, with sodium,[10] water vapor and carbon dioxide being detected.[12]

WASP-94Bb is a non-transiting planet that has been detected only by radial velocity, so it has no measured radius and true mass. Its minimum mass is 62% the mass of Jupiter.[3]

The WASP-94 A planetary system[3]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination
(°) 		Radius
b 0.452+0.035
−0.032 MJ 		0.055±0.001 3.9501907+0.0000044
−0.0000030 		<0.064[13] 88.7±0.7 1.72+0.06
−0.05 RJ
The WASP-94 B planetary system[3]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination
(°) 		Radius
b ≥0.618+0.028
−0.029 MJ 		0.0335+0.0006
−0.0005 		2.00839±0.00024 0 — —

See also

Other systems with multiple planet-hosting stars:

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. ^ a b c d e f 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. ^ a b c d e f g h i j k l m n o p q r s Neveu-VanMalle, M.; Queloz, D.; et al. (December 2014). "WASP-94 A and B planets: hot-Jupiter cousins in a twin-star system". Astronomy & Astrophysics. 572: A49. arXiv:1409.7566. Bibcode:2014A&A...572A..49N. doi:10.1051/0004-6361/201424744.
  4. ^ a b c d e f 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.
  5. ^ Ayres, Thomas (2023). "In the Trenches of the Solar-Stellar Connection. VII. Wilson-Bappu 2022". The Astrophysical Journal Supplement Series. 266 (1): 6. Bibcode:2023ApJS..266....6A. doi:10.3847/1538-4365/acb535.
  6. ^ a b c d e f g h i Teske, Johanna K.; Khanal, Sandhya; Ramírez, Ivan (March 2016). "The Curious Case of Elemental Abundance Differences in the Dual Hot Jupiter Hosts WASP-94A and B". The Astrophysical Journal. 819 (1): 19. arXiv:1601.01731. Bibcode:2016ApJ...819...19T. doi:10.3847/0004-637X/819/1/19.
  7. ^ 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.
  8. ^ "CD-34 14724A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 18 May 2025.
  9. ^ "CD-34 14724B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 18 May 2025.
  10. ^ a b Ahrer, E.; Wheatley, P. J.; et al. (March 2022). "LRG-BEASTS: Sodium absorption and Rayleigh scattering in the atmosphere of WASP-94A b using NTT/EFOSC2". Monthly Notices of the Royal Astronomical Society. 510 (4): 4857–4871. arXiv:2201.02212. Bibcode:2022MNRAS.510.4857A. doi:10.1093/mnras/stab3805.
  11. ^ Ahrer, E.; Seidel, J. V.; et al. (May 2024). "Atmospheric characterization and tighter constraints on the orbital misalignment of WASP-94 A b with HARPS". Monthly Notices of the Royal Astronomical Society. 530 (3): 2749–2759. arXiv:2404.06550. Bibcode:2024MNRAS.530.2749A. doi:10.1093/mnras/stae1000.
  12. ^ Ahrer, Eva-Maria; Gandhi, Siddharth; et al. (May 2025). "Tracing the formation and migration history: molecular signatures in the atmosphere of misaligned hot Jupiter WASP-94Ab using JWST NIRSpec/G395H". Monthly Notices of the Royal Astronomical Society. 540 (3): 2535–2554. arXiv:2505.11224. doi:10.1093/mnras/staf819.
  13. ^ Bonomo, A. S.; Desidera, S.; et al. (June 2017). "The GAPS Programme with HARPS-N at TNG. XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy & Astrophysics. 602: A107. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882.

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