WASP-64

WASP-64 / Atakoraka
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Canis Major
Right ascension 06h 44m 27.6052s[1]
Declination −32° 51′ 30.1787″[1]
Apparent magnitude (V) 12.29[2]
Characteristics
Evolutionary stage main-sequence star
Spectral type G7[2]
Apparent magnitude (J) 11.368 [1]
Apparent magnitude (G) 12.5257 [1]
Apparent magnitude (H) 11.079 [1]
Astrometry
Radial velocity (Rv)35.48 km/s
Proper motion (μ) RA: -19.389[3] mas/yr
Dec.: -1.123[3] mas/yr
Parallax (π)2.6745 ± 0.0218 mas[3]
Distance1,220 ± 10 ly
(374 ± 3 pc)
Details[4]
Mass0.993+0.034
−0.037 M☉
Radius1.036+0.046
−0.065 R☉
Luminosity0.90±0.15 L☉
Temperature5400±100[2] K
Metallicity [Fe/H]-0.08±0.11 dex
Rotation15.8±3.7 d[5]
Age3.554±1.629[5] Gyr
Other designations
Atakoraka, Gaia DR2 5583523425437258240, GSC 07091-01514, 2MASS J06442760-3251302[1]
Database references
SIMBADdata

WASP-64 is a star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. It is younger than the Sun at 3.6±1.6 billion years,[5] and it has a metal abundance similar to the Sun.[2] The star is rotating rapidly, being spun up by the giant planet in a close orbit.[5]

WASP-64 was named Atakoraka in 2019 after the Atacora, the largest mountain range in Togo.[6] An imaging survey in 2017 failed to find any stellar companions.[7]

  1. ^ a b c d e f Cite error: The named reference simbad was invoked but never defined (see the help page).
  2. ^ a b c d WASP-64 The planetary system WASP-64 hosts at least one planet
  3. ^ a b c 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.
  4. ^ Cite error: The named reference Gillon2012 was invoked but never defined (see the help page).
  5. ^ a b c d 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
  6. ^ Cite error: The named reference Methodology was invoked but never defined (see the help page).
  7. ^ 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. (2018), "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