WASP-57 is a single G-type main-sequence star about 1310 light-years away. WASP-57 is depleted in heavy elements, having 55% of the solar abundance of iron.[3] WASP-57 is much younger than the Sun at 0.957±0.518 billion years.[5]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Libra |
| Right ascension | 14h 55m 16.8229s[1] |
| Declination | −02° 03′ 27.5991″[1] |
| Apparent magnitude (V) | 13.04 |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | G6[2] |
| Astrometry | |
| Radial velocity (Rv) | -23.290[1] km/s |
| Proper motion (μ) | RA: -27.064[1] mas/yr Dec.: -4.687[1] mas/yr |
| Parallax (π) | 2.4826 ± 0.0359 mas[1] |
| Distance | 1,310 ± 20 ly (403 ± 6 pc) |
| Details[3] | |
| Mass | 0.886±0.061 M☉ |
| Radius | 0.927±0.031 R☉ |
| Surface gravity (log g) | 4.452±0.024[4] cgs |
| Temperature | 5600±100 K |
| Metallicity [Fe/H] | -0.25±0.1 dex |
| Rotation | 12.7±4.5[5] |
| Rotational velocity (v sin i) | 3.7±1.3 km/s |
| Age | 0.957±0.518[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
A multiplicity survey in 2015 did not detect any stellar companions to WASP-57.[6]
Planetary system
editIn 2012 a transiting hot Jupiter planet b was detected on a tight, circular orbit around WASP-57.[7]
Planetary equilibrium temperature is 1338±29 K.[4]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.643+0.056 −0.054 MJ |
0.03772+0.00083 −0.00089 |
2.83891856±0.00000081 | <0.059 | 86.05±0.20° | 1.050±0.052 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 "WASP-57". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ a b c Bonomo, A. S.; et al. (2017), "The GAPS Programme with HARPS-N at TNG", Astronomy & Astrophysics, 602: A107, arXiv:1704.00373, Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID 118923163
- ^ a b Southworth, John; et al. (2015), "Larger and faster: Revised properties and a shorter orbital period for the WASP-57 planetary system from a pro-am collaboration", Monthly Notices of the Royal Astronomical Society, 454 (3): 3094–3107, arXiv:1509.05609, doi:10.1093/mnras/stv2183
- ^ a b c Gallet, F.; Gallet (2020), "TATOO: Tidal-chronology standalone tool to estimate the age of massive close-in planetary systems", Astronomy & Astrophysics, 641: A38, arXiv:2006.07880, Bibcode:2020A&A...641A..38G, doi:10.1051/0004-6361/202038058, S2CID 219687851
- ^ Wöllert, Maria; Brandner, Wolfgang (2015), "A Lucky Imaging search for stellar sources near 74 transit hosts", Astronomy & Astrophysics, 579: A129, arXiv:1506.05456, Bibcode:2015A&A...579A.129W, doi:10.1051/0004-6361/201526525, S2CID 118903879
- ^ Faedi, F.; 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, Bibcode:2013A&A...551A..73F, doi:10.1051/0004-6361/201220520, S2CID 14346225
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