Astronomy:HAT-P-27
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.[1] 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″[2] and proven to be physically bound to the system in 2016.[3]
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.[1] 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.[4] No orbital decay was detected as of 2018, despite the close proximity of the planet to the star.[5]
The presence of an additional planet in the system has been suspected since 2015.[6]
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.[7]
Template:Orbitbox planet hypothetical| 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[4]° | 1.038+0.077−0.058 RJ |
References
- ↑ 1.0 1.1 1.2 Béky, B.; Bakos, G. Á.; Hartman, J.; Torres, G.; Latham, D. W.; Jordán, A.; Arriagada, P.; Bayliss, D. et al. (2011). "HAT-P-27b: A Hot Jupiter Transiting a G Star on a 3 Day Orbit". The Astrophysical Journal 734 (2): 109. doi:10.1088/0004-637X/734/2/109. Bibcode: 2011ApJ...734..109B.
- ↑ Wöllert, Maria; Brandner, Wolfgang (2015). "A Lucky Imaging search for stellar sources near 74 transit hosts". Astronomy & Astrophysics 579: A129. doi:10.1051/0004-6361/201526525. Bibcode: 2015A&A...579A.129W.
- ↑ Ngo, Henry; Knutson, Heather A.; Hinkley, Sasha; Bryan, Marta; Crepp, Justin R.; Batygin, Konstantin; Crossfield, Ian; Hansen, Brad et al. (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. doi:10.3847/0004-637X/827/1/8. Bibcode: 2016ApJ...827....8N.
- ↑ 4.0 4.1 Brown, D. J. A.; Collier Cameron, A.; Díaz, R. F.; Doyle, A. P.; Gillon, M.; Lendl, M.; Smalley, B.; Triaud, A. H. M. J. et al. (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. doi:10.1088/0004-637X/760/2/139. Bibcode: 2012ApJ...760..139B.
- ↑ 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. doi:10.3847/1538-3881/aaaf71. PMID 31080254. Bibcode: 2018AJ....155..165P.
- ↑ 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. doi:10.1093/mnras/stv1187. Bibcode: 2015MNRAS.451.4060S.
- ↑ 7.0 7.1 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. doi:10.1093/mnras/stae1740.
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14h 51m 04.1870s, +05° 56′ 50.5482″
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