HAT-P-27

Last updated
HAT-P-27
Observation data
Epoch J2000       Equinox J2000
Constellation Virgo [1]
Right ascension 14h 51m 04.1870s [2]
Declination +05° 56′ 50.549″ [2]
Apparent magnitude  (V)12.214 [3]
Characteristics
Evolutionary stage main-sequence star [4]
Spectral type G8 [4]
Astrometry
Radial velocity (Rv)−16.74±0.56 [2] km/s
Proper motion (μ)RA: −28.610(19) mas/yr [2]
Dec.: −2.774(19) mas/yr [2]
Parallax (π)4.9528±0.0169  mas [2]
Distance 659 ± 2  ly
(201.9 ± 0.7  pc)
Orbit [5]
PrimaryHAT-P-27
CompanionHAT-P-27 B
Semi-major axis (a)0.656±0.021"
(131 AU)
Details [3]
Mass 0.945±0.035  M☉
Radius 0.898+0.054
−0.039  R☉
Luminosity 0.57+0.09
−0.07  L☉
Surface gravity (log g)4.51±0.04  cgs
Temperature 5300±90  K
Metallicity [Fe/H]0.29±0.10  dex
Rotation 0.4±0.4
Rotational velocity (v sin i)0.6+0.7
−0.4 [6]  km/s
Age 4.4+3.8
−2.6  Gyr
Other designations
HAT-P-27, TOI-5672, TIC 461239485, WASP-40, GSC 00333-00351, 2MASS J14510418+0556505 [7]
Database references
SIMBAD data
Exoplanet Archive data

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. [3] HAT-P-27 is enriched in heavy elements, having a 195% concentration of iron compared to the Sun.

A very dim stellar companion was detected in 2015 at a projected separation of 0.656″ [5] and proven to be physically bound to the system in 2016. [4]

Planetary system

In 2011 a transiting hot Jupiter type planet b was detected in a mildly eccentric orbit. The planetary equilibrium temperature is 1207±41 K. [3] A survey in 2013 failed to find any Rossiter-McLaughlin effect and therefore was unable to constrain the inclination of planetary orbit to the equatorial plane of the parent star. [6] No orbital decay was detected as of 2018, despite the close proximity of the planet to the star. [8]

The presence of an additional planet in the system has been suspected since 2015. [9]

In 2024, a detection of a possible Neptune-like planet was reported. It is expected to be an analog of Neptune in terms of radius, although much hotter due to the low orbital separation; one year on this planet lasts one day and five hours, causing the planetary equilibrium temperature to be 1,426  K (1,153 °C). More observations are needed to validate its existence. [10]

The HAT-P-27 planetary system [3] [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b0.660±0.033  MJ 0.0403±0.00053.039586±0.0000120.078±0.04785.0±0.2 [6] ° 1.038+0.077
−0.058  RJ
c(unconfirmed)17.8+13.8
−0.81 M🜨 		—1.1994(2)<0.19—4.33±0.44  R🜨

References

  1. ↑ 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.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 4 5 Béky, B.; Bakos, G. Á.; Hartman, J.; Torres, G.; Latham, D. W.; Jordán, A.; Arriagada, P.; Bayliss, D.; Kiss, L. L.; Kovács, Géza; Quinn, S. N.; Marcy, G. W.; Howard, A. W.; Fischer, D. A.; Johnson, J. A.; Esquerdo, G. A.; Noyes, R. W.; Buchhave, L. A.; Sasselov, D. D.; Stefanik, R. P.; Perumpilly, G.; Lázár, J.; Papp, I.; Sári, P. (2011). "HAT-P-27b: A Hot Jupiter Transiting a G Star on a 3 Day Orbit". The Astrophysical Journal. 734 (2): 109. arXiv: 1101.3511 . Bibcode:2011ApJ...734..109B. doi:10.1088/0004-637X/734/2/109. S2CID   31357299.
  4. 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.
  5. 1 2 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.
  6. 1 2 3 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.
  7. ↑ "HAT-P-27". SIMBAD . Centre de données astronomiques de Strasbourg.
  8. ↑ Penev, Kaloyan; Bouma, L. G.; Winn, Joshua N.; Hartman, Joel D. (2018). "Empirical Tidal Dissipation in Exoplanet Hosts from Tidal Spin-up". The Astronomical Journal. 155 (4): 165. arXiv: 1802.05269 . Bibcode:2018AJ....155..165P. doi: 10.3847/1538-3881/aaaf71 . PMC   6510550 . PMID   31080254. S2CID   64370118.
  9. ↑ Seeliger, M.; et al. (2015). "Ground-based transit observations of the HAT-P-18, HAT-P-19, HAT-P-27/WASP40 and WASP-21 systems". Monthly Notices of the Royal Astronomical Society. 451 (4): 4060. arXiv: 1508.06215 . Bibcode:2015MNRAS.451.4060S. doi: 10.1093/mnras/stv1187 .
  10. 1 2 Dévora-Pajares, Martín; Pozuelos, Francisco J.; Thuillier, Antoine; Timmermans, Mathilde; Van Grootel, Valérie; Bonidie, Victoria; Mota, Luis Cerdeño; Suárez, Juan C. (2024). "The SHERLOCK pipeline: new exoplanet candidates in the WASP-16, HAT-P-27, HAT-P-26, and TOI-2411 systems". Monthly Notices of the Royal Astronomical Society . 532 (4): 4752–4773. arXiv: 2407.14602 . doi: 10.1093/mnras/stae1740 .
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