HAT-P-27
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 14h 51m 04.1870s[1] |
| Declination | +05° 56′ 50.5482″[1] |
| Apparent magnitude (V) | 12.214[2] |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | G8 |
| Astrometry | |
| Radial velocity (Rv) | -15.901[1] km/s |
| Proper motion (μ) | RA: -28.621[1] mas/yr Dec.: -2.757[1] mas/yr |
| Parallax (π) | 4.9922 ± 0.0360 mas[3] |
| Distance | 653 ± 5 ly (200 ± 1 pc) |
| Orbit[4] | |
| Primary | HAT-P-27 |
| Companion | HAT-P-27 B |
| Semi-major axis (a) | 0.656±0.021" (131 AU) |
| Details[2] | |
| 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[5] km/s |
| Age | 4.4+3.8 −2.6 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HAT-P-27, also known as WASP-40, is the primary of a binary star system about 650 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]
Planetary system
In 2011 a transiting hot Jupiter planet b was detected on a mildly eccentric orbit. The planetary equilibrium temperature is 1207±41 K.[2] The survey in 2013 has failed to find any Rossiter-McLaughlin effect effect and therefore was unable to constrain the inclination of planetary orbit to the equatorial plane of the parent star.[5] No orbital decay was detected as in 2018, despite of the close proximity of the planet to the star.[7]
Additional planet in the system is suspected since 2015.[8]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.660±0.033 MJ | 0.0403±0.0005 | 3.039586±0.000012 | 0.078±0.047 | 85.0±0.2[5]° | 1.038+0.077 −0.058 RJ |
References
- ^ a b c d e f "HAT-P-27". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ a b c d e 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, doi:10.1088/0004-637X/734/2/109, S2CID 31357299
- ^ 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.
- ^ 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, doi:10.1051/0004-6361/201526525, S2CID 118903879
- ^ a b c 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, doi:10.1088/0004-637X/760/2/139, S2CID 54033638
- ^ 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: 8, arXiv:1606.07102, doi:10.3847/0004-637X/827/1/8, S2CID 41083068
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ 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, doi:10.3847/1538-3881/aaaf71, PMID 31080254, S2CID 64370118
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ Ground-based transit observations of the HAT-P-18,HAT-P-19, HAT-P-27/WASP40 and WASP-21 systems
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