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WASP-54

WASP-54
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]
Distance830 ± 10 ly
(253 ± 4 pc)
Orbit[3]
PrimaryWASP-54A
CompanionWASP-54B
Semi-major axis (a)5.728±0.006"
(1450 AU)
Details[4]
WASP-54A
Mass1.213±0.032 M☉
Radius1.828+0.091
−0.081 R☉
Surface gravity (log g)4.00±0.02[5] cgs
Temperature6100±100 K
Metallicity [Fe/H]-0.27±0.08 dex
Rotational velocity (v sin i)4.0±0.8 km/s
Age6.9+1.0
−1.9 Gyr
WASP-54B
Mass0.19±0.01[3] M☉
Temperature3216+26
−25[3] K
Other designations
BD+00 3088, Gaia DR2 3661983850663908608, TYC 4967-678-1, GSC 04967-00678, 2MASS J13414903-0007410[2]
Database references
SIMBADdata

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]

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

In 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]

The WASP-54 planetary system[4]
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

  1. ^ 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.
  2. ^ a b "BD+00 3088". SIMBAD. Centre de données astronomiques de Strasbourg.
  3. ^ 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
  4. ^ 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
  5. ^ Correcting the spectroscopic surface gravity using transits and asteroseismology No significant effect on temperatures or metallicities with ARES and MOOG in local thermodynamic equilibrium
  6. ^ 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
  7. ^ 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


Quelle: https://en.wikipedia.org/wiki/WASP-54