WASP-58

WASP-58
Observation data
Epoch J2000      Equinox J2000
Constellation Lyra
Right ascension 18h 18m 48.2531s[1]
Declination 45° 10′ 19.2592″[1]
Apparent magnitude (V) 11.66[2]
Characteristics
Evolutionary stage Main sequence
Spectral type G2V[2]
Astrometry
Radial velocity (Rv)-28.708[1] km/s
Proper motion (μ) RA: 32.579[1] mas/yr
Dec.: 47.140[1] mas/yr
Parallax (π)3.4147 ± 0.0214 mas[1]
Distance955 ± 6 ly
(293 ± 2 pc)
Orbit[3]
PrimaryWASP-58A
CompanionWASP-58B
Semi-major axis (a)1.281±0.002"
(384±64 AU)
Details[4]
WASP-58A
Mass0.940±0.100 M☉
Radius1.17±0.13 R☉
Surface gravity (log g)4.23±0.1[5] cgs
Temperature6039±55[5] K
Metallicity [Fe/H]-0.09±0.04 dex
Rotation22.6+11.7
−6.1 d[6]
Rotational velocity (v sin i)2.8±0.9 km/s
Age12.80+0.20
−2.10 Gyr
WASP-58B
Temperature3396±53[3] K
Other designations
Gaia DR2 2115245554756763392, TYC 3525-76-1, 2MASS J18184825+4510192[7]
Database references
SIMBADdata

WASP-58 is a binary star system comprising a G-type main-sequence star and a red dwarf about 955 light-years away. WASP-58 is slightly depleted in heavy elements, having 80% of the solar abundance of iron.[5] WASP-58 is much older than the Sun at 12.80+0.20
−2.10 billion years.[4]

Lithium was detected in the stellar spectrum of WASP-58A, making the star anomalous for its advanced age.[2]

A multiplicity survey in 2015 did detect a red dwarf stellar companion[8] at a projected separation of 1.281±0.002″ to WASP-58A, and it was confirmed to be gravitationally bound in 2016.[3]

  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 c Cite error: The named reference Hebrard2012 was invoked but never defined (see the help page).
  3. ^ a b c 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
  4. ^ a b Cite error: The named reference Bonomo2017 was invoked but never defined (see the help page).
  5. ^ a b c 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
  6. ^ 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
  7. ^ Cite error: The named reference simbad was invoked but never defined (see the help page).
  8. ^ 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