WASP-54, also known as BD+00 3088, is a binary star system about 825 light-years away. The primary, WASP-54A, is a F-type main-sequence star, accompanied by the red dwarf WASP-54B on a wide orbit. WASP-54 is depleted in heavy elements, having 55% of the solar abundance of iron.[4] The age of WASP-54 is slightly older than the Sun's at 6.9+1.0
−1.9 billion years.[4]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 13h 41m 49.0302s[1] |
| Declination | −00° 07′ 41.0337″[1] |
| Apparent magnitude (V) | 10.41 |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | F8[2] |
| Astrometry | |
| Radial velocity (Rv) | -2.82[1] km/s |
| Proper motion (μ) | RA: -24.685[1] mas/yr Dec.: -4.687[1] mas/yr |
| Parallax (π) | 3.9522 ± 0.0692 mas[1] |
| Distance | 830 ± 10 ly (253 ± 4 pc) |
| Orbit[3] | |
| Primary | WASP-54A |
| Companion | WASP-54B |
| Semi-major axis (a) | 5.728±0.006" (1450 AU) |
| Details[4] | |
| WASP-54A | |
| Mass | 1.213±0.032 M☉ |
| Radius | 1.828+0.091 −0.081 R☉ |
| Surface gravity (log g) | 4.00±0.02[5] cgs |
| Temperature | 6100±100 K |
| Metallicity [Fe/H] | -0.27±0.08 dex |
| Rotational velocity (v sin i) | 4.0±0.8 km/s |
| Age | 6.9+1.0 −1.9 Gyr |
| WASP-54B | |
| Mass | 0.19±0.01[3] M☉ |
| Temperature | 3216+26 −25[3] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
A multiplicity survey in 2017 did detect a red dwarf stellar companion WASP-54B 5.7″ away from WASP-54A.[6] The companion was proven to be co-moving in 2020.[3]
Planetary system
editIn 2012 a transiting hot Jupiter planet b was detected on a tight, mildly eccentric[4] orbit around WASP-54A.[7]
Planetary equilibrium temperature is 1742+49
−69 K.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.606±0.018 MJ | 0.04988+0.00043 −0.00045 |
3.6936411±0.0000059 | <0.06 | 84.97±0.61° | 1.653+0.090 −0.083 RJ |
References
edit- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b "BD+00 3088". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ a b c d 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
- ^ a b c d e Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A.; Lodato, G.; Marzari, F.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Covino, E.; Gratton, R.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Affer, L.; Biazzo, K.; Bignamini, A.; Esposito, M.; Giacobbe, P.; Hébrard, G.; Malavolta, L.; et al. (2017), "The GAPS Programme with HARPS-N@TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets", Astronomy & Astrophysics, A107: 602, arXiv:1704.00373, Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID 118923163
- ^ Correcting the spectroscopic surface gravity using transits and asteroseismology No significant effect on temperatures or metallicities with ARES and MOOG in local thermodynamic equilibrium
- ^ Evans, D. F.; Southworth, J.; Smalley, B.; Jørgensen, U. G.; Dominik, M.; Andersen, M. I.; Bozza, V.; Bramich, D. M.; Burgdorf, M. J.; Ciceri, S.; d'Ago, G.; Figuera Jaimes, R.; Gu, S.-H.; Hinse, T. C.; Henning, Th.; Hundertmark, M.; Kains, N.; Kerins, E.; Korhonen, H.; Kokotanekova, R.; Kuffmeier, M.; Longa-Peña, P.; Mancini, L.; MacKenzie, J.; Popovas, A.; Rabus, M.; Rahvar, S.; Sajadian, S.; Snodgrass, C.; et al. (2017), "High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP). II. Lucky Imaging results from 2015 and 2016", Astronomy & Astrophysics, 610: A20, arXiv:1709.07476, Bibcode:2018A&A...610A..20E, doi:10.1051/0004-6361/201731855, S2CID 53400492
- ^ a b Faedi, F.; Pollacco, D.; Barros, S. C. C.; Brown, D.; Collier Cameron, A.; Doyle, A. P.; Enoch, R.; Gillon, M.; Gómez Maqueo Chew, Y.; Hébrard, G.; Lendl, M.; Liebig, C.; Smalley, B.; Triaud, A. H. M. J.; West, R. G.; Wheatley, P. J.; Alsubai, K. A.; Anderson, D. R.; Armstrong, D.; Bento, J.; Bochinski, J.; Bouchy, F.; Busuttil, R.; Fossati, L.; Fumel, A.; Haswell, C. A.; Hellier, C.; Holmes, S.; Jehin, E.; et al. (2012), "WASP-54b, WASP-56b and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP", Astronomy & Astrophysics, 551: A73, arXiv:1210.2329, doi:10.1051/0004-6361/201220520, S2CID 14346225