WASP-76

WASP-76

Artist impression of WASP-76b and WASP-76
Observation data
Epoch J2000      Equinox ICRS
Constellation Pisces
Right ascension 01h 46m 31.8576s
Declination 02° 42′ 02.030″
Apparent magnitude (V) 9.52
Characteristics
Evolutionary stage main sequence
Spectral type F7
B−V color index 0.61
J−H color index 0.21
J−K color index 0.3
Astrometry
Radial velocity (Rv)−1.152±0.0033 km/s
Proper motion (μ) RA: +45.531 mas/yr
Dec.: −40.593 mas/yr
Parallax (π)5.2899±0.0826 mas
Distance617 ± 10 ly
(189 ± 3 pc)
Orbit
Period (P)903+316
−416 yr
Semi-major axis (a)118+27
−39 au
Eccentricity (e)0.844+0.123
−0.062
Inclination (i)65.7+13.0
−8.8°
Longitude of the node (Ω)28+8
−9°
Periastron epoch (T)2,152,623+148,144
−111,734 BJD
Argument of periastron (ω)
(secondary)		333+24
−27°
Details
A
Mass1.372+0.031
−0.030 M☉
Radius1.667±0.020 R☉
Luminosity4.6 L☉
Surface gravity (log g)4.4±0.1 cgs
Temperature6,250±100 K
Metallicity [Fe/H]0.23±0.1 dex
Rotational velocity (v sin i)3.3±0.6 km/s
Age5.3+6.1
−2.9 Gyr
B
Mass0.672+0.031
−0.030 M☉
Other designations
WASP-76, 2MASS J01463185+0242019, Gaia DR3 2512326349403275520
Database references
SIMBADdata

WASP-76, also known as BD+01 316, is a binary star in the constellation of Pisces. The primary is a yellow-white main sequence star, with a mass around 1.37 M☉. The stellar companion has a mass of 0.67 M☉. Both take around 900 years to orbit around each other. The companion was first reported in 2014.

After about five billion years, WASP-76 A has expanded and become more luminous than at the start of its main sequence life, but most probably has not yet reached the subgiant branch.

Planetary system

Size comparison of WASP-76 b, Jupiter and Saturn
Artistic image of WASP-76b, showing its possible glory effect

The "hot Jupiter" class planet WASP-76b was discovered around WASP-76 in 2013.

Analysis of transit-timing variations suggest an additional planet in the system.

The WASP-76 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination
(°)		 Radius
b 0.92 MJ 0.0316±0.0002 1.80988132(12) 0.00087±0.00031 87.88±0.16 1.842±0.024 RJ

References

  1. ↑ "Gemini North Detects Multiple Rock-Forming Elements in the Atmosphere of a Scorching Exoplanet" (Press release). NOIRLab. 2023-06-14. Retrieved 2025-06-13.
  2. ↑ 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.
  3. 1 2 3 4 5 6 7 8 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.
  4. ↑ 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.
  5. 1 2 3 4 5 6 7 8 West, R. G.; Hellier, C.; Almenara, J.-M.; Anderson, D. R.; Barros, S. C. C.; Bouchy, F.; Brown, D. J. A.; Collier Cameron, A.; Deleuil, M.; Delrez, L.; Doyle, A. P.; Faedi, F.; Fumel, A.; Gillon, M.; Gómez Maqueo Chew, Y.; Hébrard, G.; Jehin, E.; Lendl, M.; Maxted, P. F. L.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Smalley, B.; Smith, A. M. S.; Southworth, J.; Triaud, A. H. M. J.; Udry, S. (2016). "Three irradiated and bloated hot Jupiters". Astronomy & Astrophysics. 585: A126. arXiv:1310.5607. doi:10.1051/0004-6361/201527276. S2CID 54746373.
  6. ↑ Soubiran, C.; Jasniewicz, G.; Chemin, L.; Zurbach, C.; Brouillet, N.; Panuzzo, P.; Sartoretti, P.; Katz, D.; Le Campion, J. -F.; Marchal, O.; Hestroffer, D.; Thévenin, F.; Crifo, F.; Udry, S.; Cropper, M.; Seabroke, G.; Viala, Y.; Benson, K.; Blomme, R.; Jean-Antoine, A.; Huckle, H.; Smith, M.; Baker, S. G.; Damerdji, Y.; Dolding, C.; Frémat, Y.; Gosset, E.; Guerrier, A.; Guy, L. P.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID 52952408.
  7. 1 2 3 4 Morgan, Marvin; Xuan, Jerry W.; Bowler, Brendan P.; Franson, Kyle; Liu, Michael C.; Batygin, Konstantin; Knutson, Heather A.; Benneke, Björn; Cronin, Julianne (2026-10-13). "Tracing the Influence of Distant companions on Exoplanetary Systems (TIDES) I. Highly Eccentric and Misaligned Binary Companions to Hot Jupiters". The Astronomical Journal. arXiv:2610.17811.
  8. 1 2 3 Wang, Weilong; Gu, Shenghong; Wang, Xiaobin; Sun, Leilei; Lee, Byeong-Cheol; Kwok, Chi-Tai; Hui, Ho-Keung; Dou, Jiangpei; Xiang, Yue; Cao, Dongtao; Xu, Fukun (June 2025). "Observations and Studies on the Transiting Systems HAT-P-36, XO-2 and WASP-76". The Astronomical Journal. 169 (6): 342. Bibcode:2025AJ....169..342W. doi:10.3847/1538-3881/add1de. ISSN 0004-6256.
  9. ↑ Ngo, Henry; Knutson, Heather A.; Hinkley, Sasha; Bryan, Marta; Crepp, Justin R.; Batygin, Konstantin; Crossfield, Ian; Hansen, Brad; Howard, Andrew W.; Johnson, John A.; Mawet, Dimitri; Morton, Timothy D.; Muirhead, Philip S.; Wang, Ji (2016). "Friends of Hot Jupiters. IV. Stellar Companions Beyond 50 au Might Facilitate Giant Planet Formation, but Most are Unlikely to Cause Kozai-Lidov Migration". The Astrophysical Journal. 827 (1): 8. arXiv:1606.07102. Bibcode:2016ApJ...827....8N. doi:10.3847/0004-637X/827/1/8.