HAT-P-27

HAT-P-27
Observation data
Epoch J2000      Equinox J2000
Constellation Virgo
Right ascension 14h 51m 04.1870s[1]
Declination +05° 56′ 50.549″[1]
Apparent magnitude (V) 12.214[2]
Characteristics
Evolutionary stage main-sequence star
Spectral type G8
Astrometry
Radial velocity (Rv)-15.901[3] km/s
Proper motion (μ) RA: −28.610(19) mas/yr[1]
Dec.: −2.774(19) mas/yr[1]
Parallax (π)4.952 ± 0.0169 mas[1]
Distance659 ± 2 ly
(201.9 ± 0.7 pc)
Orbit[4]
PrimaryHAT-P-27
CompanionHAT-P-27 B
Semi-major axis (a)0.656±0.021"
(131 AU)
Details[2]
Mass0.945±0.035 M☉
Radius0.898+0.054
−0.039 R☉
Luminosity0.57+0.09
−0.07 L☉
Surface gravity (log g)4.51±0.04 cgs
Temperature5300±90 K
Metallicity [Fe/H]0.29±0.10 dex
Rotation0.4±0.4
Rotational velocity (v sin i)0.6+0.7
−0.4[5] km/s
Age4.4+3.8
−2.6 Gyr
Other designations
HAT-P-27, Gaia DR2 1159336403336463872, WASP-40, GSC 00333-00351, 2MASS J14510418+0556505[3]
Database references
SIMBADdata

HAT-P-27, also known as WASP-40, is the primary of a binary star system about 659 light-years away. It is a G-type main-sequence star. The star's age is similar to the Sun's at 4.4 billion years.[2] HAT-P-27 is enriched in heavy elements, having a 195% concentration of iron compared to the Sun.

The very dim stellar companion was detected in 2015 at a projected separation of 0.656″[4] and proven to be physically bound to the system in 2016.[6]

  1. ^ a b c d Cite error: The named reference Gaia DR3 was invoked but never defined (see the help page).
  2. ^ a b c Cite error: The named reference Beky2011 was invoked but never defined (see the help page).
  3. ^ a b Cite error: The named reference simbad was invoked but never defined (see the help page).
  4. ^ a b 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
  5. ^ Brown, D. J. A.; Collier Cameron, A.; Díaz, R. F.; Doyle, A. P.; Gillon, M.; Lendl, M.; Smalley, B.; Triaud, A. H. M. J.; Anderson, D. R.; Enoch, B.; Hellier, C.; Maxted, P. F. L.; Miller, G. R. M.; Pollacco, D.; Queloz, D.; Boisse, I.; Hébrard, G. (2013), "Analysis of Spin-Orbit Alignment in the Wasp-32, Wasp-38, and Hat-P-27/Wasp-40 Systems", The Astrophysical Journal, 760 (2): 139, arXiv:1303.5649, Bibcode:2012ApJ...760..139B, doi:10.1088/0004-637X/760/2/139, S2CID 54033638
  6. ^ 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