Astronomy:WASP-54
Observation data Equinox J2000.0]] (ICRS) | |
---|---|
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[1] mas |
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 |
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]
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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 "BD+00 3088". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=BD%2B00+3088.
- ↑ 3.0 3.1 3.2 3.3 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, doi:10.1051/0004-6361/201937127, Bibcode: 2020A&A...635A..73B
- ↑ 4.0 4.1 4.2 4.3 4.4 Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A. 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, doi:10.1051/0004-6361/201629882, Bibcode: 2017A&A...602A.107B
- ↑ 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. et al. (2017), "High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP). II. Lucky Imaging results from 2015 and 2016", Astronomy & Astrophysics 610: A20, doi:10.1051/0004-6361/201731855, Bibcode: 2018A&A...610A..20E
- ↑ 7.0 7.1 Faedi, F.; Pollacco, D.; Barros, S. C. C.; Brown, D.; Collier Cameron, A.; Doyle, A. P.; Enoch, R.; Gillon, M. et al. (2012), "WASP-54b, WASP-56b and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP", Astronomy & Astrophysics 551: A73, doi:10.1051/0004-6361/201220520
Coordinates: 13h 41m 49.0302s, −00° 07′ 41.0337″
Original source: https://en.wikipedia.org/wiki/WASP-54.
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