WASP-58
(Redirected from WASP-58b)
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Lyra[1] |
| Right ascension | 18h 18m 48.25296s[2] |
| Declination | +45° 10′ 19.2603″[2] |
| Apparent magnitude (V) | 11.66[3] |
| Characteristics | |
| Evolutionary stage | Main sequence[2] |
| Spectral type | G2V[3] |
| Astrometry | |
| Radial velocity (Rv) | −28.42±0.71[2] km/s |
| Proper motion (μ) | RA: 32.658 mas/yr[2] Dec.: 47.057 mas/yr[2] |
| Parallax (π) | 3.3963±0.0112 mas[2] |
| Distance | 960 ± 3 ly (294.4 ± 1.0 pc) |
| Orbit[4] | |
| Primary | WASP-58A |
| Name | WASP-58B |
| Semi-major axis (a) | 1.281±0.002" (384±64 AU) |
| Details[5] | |
| WASP-58A | |
| Mass | 0.940±0.100 M☉ |
| Radius | 1.17±0.13 R☉ |
| Surface gravity (log g) | 4.23±0.1[6] cgs |
| Temperature | 6039±55[6] K |
| Metallicity [Fe/H] | -0.09±0.04 dex |
| Rotation | 22.6+11.7 −6.1 d[7] |
| Rotational velocity (v sin i) | 2.8±0.9 km/s |
| Age | 12.80+0.20 −2.10 Gyr |
| WASP-58B | |
| Temperature | 3396±53[4] K |
| Other designations | |
| TOI-1627, TIC 424435940, WASP-58, TYC 3525-76-1, 2MASS J18184825+4510192[8] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
WASP-58 is a binary star system in the constellation Lyra. It comprises a G-type main-sequence star and a red dwarf at a separation of 384 astronomical units. WASP-58 is slightly depleted in heavy elements, having 80% of the solar abundance of iron. The system is much older than the Sun at 12.80+0.20
−2.10 billion years. Based on parallax measurements, it lies at a distance of 960 light-years (290 parsecs).
Lithium was detected in the stellar spectrum of WASP-58A, making the star anomalous for its advanced age.[3]
A multiplicity survey in 2015 detected a red dwarf stellar companion[9] at a projected separation of 1.281±0.002″ to WASP-58A, and it was confirmed to be gravitationally bound in 2016.[4]
Planetary system
[edit]In 2012 a transiting hot Jupiter planet, WASP-58b, was detected on a tight, circular orbit around the primary star WASP-58A.[3] The planetary equilibrium temperature is 1270±80 K.[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| b | 0.899+0.074 −0.072 MJ |
0.0562+0.0019 −0.0020 |
5.017180±0.000011 | <0.044 | 87.4±1.5 | 1.37±0.2 RJ |
References
[edit]- ↑ 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.
- 1 2 3 4 5 6 7 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.
- 1 2 3 4 5 Hébrard, G.; et al. (2012), "WASP-52b, WASP-58b, WASP-59b, and WASP-60b: Four new transiting close-in giant planets", Astronomy & Astrophysics, 549: A134, arXiv:1211.0810, doi:10.1051/0004-6361/201220363, S2CID 54502046
- 1 2 3 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, S2CID 41083068
- 1 2 Bonomo, A. S.; 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, 602: A107, arXiv:1704.00373, Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID 118923163
- 1 2 Andreasen, D. T.; Sousa, S. G.; Tsantaki, M.; Teixeira, G. D. C.; Mortier, A.; Santos, N. C.; Suárez-Andrés, L.; Delgado-Mena, E.; Ferreira, A. C. S. (2017), "SWEET-Cat update and FASMA", Astronomy & Astrophysics, 600: A69, arXiv:1703.06671, Bibcode:2017A&A...600A..69A, doi:10.1051/0004-6361/201629967, S2CID 119534579
- ↑ Brown, D. J. A. (2014), "Discrepancies between isochrone fitting and gyrochronology for exoplanet host stars?", Monthly Notices of the Royal Astronomical Society, 442 (2): 1844–1862, arXiv:1406.4402, Bibcode:2014MNRAS.442.1844B, doi:10.1093/mnras/stu950
- ↑ "WASP-58". SIMBAD. Centre de données astronomiques de Strasbourg.
- ↑ Wöllert, Maria; Brandner, Wolfgang; Bergfors, Carolina; Henning, Thomas (2015), "A Lucky Imaging search for stellar companions to transiting planet host stars", Astronomy & Astrophysics, 575: A23, arXiv:1507.01938, Bibcode:2015A&A...575A..23W, doi:10.1051/0004-6361/201424091, S2CID 119250579