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HAT-P-20

Coordinates: Sky map 07h 27m 39.9487s, +24° 20′ 11.5183″
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HAT-P-20
Observation data
Epoch J2000      Equinox J2000
Constellation Gemini[1]
Right ascension 07h 27m 39.9489s[2]
Declination +24° 20′ 11.516″[2]
Apparent magnitude (V) 11.35[3]
Characteristics
Evolutionary stage main sequence[2]
Spectral type K3V[4]
Astrometry
Radial velocity (Rv)-18.559 km/s
Proper motion (μ) RA: −5.104(18) mas/yr[2]
Dec.: −96.090(16) mas/yr[2]
Parallax (π)14.0065±0.0176 mas[2]
Distance232.9 ± 0.3 ly
(71.40 ± 0.09 pc)
Details
Mass0.798±0.018[5] M☉
Radius0.744±0.011[5] R☉
Luminosity0.19[6] L☉
Surface gravity (log g)4.52±0.09[7] cgs
Temperature4595±45[7] K
Metallicity0.22±0.09[7]
Rotation14.66±0.03 d[5]
Rotational velocity (v sin i)2.0±0.5[7] km/s
Age334[8] Myr
Other designations
Gaia DR2 869913435026514688, 2MASS J07273995+2420118[9]
Database references
SIMBADdata

HAT-P-20 is a K-type main-sequence star about 233 light-years away. The star has a strong starspot activity,[5] and its equatorial plane is misaligned by 36+10
−12° with the planetary orbit.[7] Although star with a giant planet on close orbit is expected to be spun-up by tidal forces, only weak indications of tidal spin-up were detected.[10]

Planetary system

[edit]

In 2010 a transiting hot super-Jovian planet was detected.[4] Its equilibrium temperature is 996±19 K.

Size comparison of HAT-P-20 b and Jupiter
The HAT-P-20 planetary system[4][5][7]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 7.59±0.12 MJ 0.03671±0.00027 2.8753172±0.0000003 0.0172±0.0016 86.3±0.1° 0.952±0.017 RJ

References

[edit]
  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. ^ a b c d e 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. ^ Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)". Vizier Online Data Catalog. Bibcode:2012yCat.1322....0Z.
  4. ^ a b c Bakos, G. Á.; Hartman, J.; Torres, G.; Latham, D. W.; Kovács, Géza; Noyes, R. W.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Howard, A. W.; Kipping, D.; Esquerdo, G. A.; Shporer, A.; Béky, B.; Buchhave, L. A.; Perumpilly, G.; Everett, M.; Sasselov, D. D.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P. (2010). "HAT-P-20b–HAT-P-23b: FOUR MASSIVE TRANSITING EXTRASOLAR PLANETS". The Astrophysical Journal. 742 (2): 116. arXiv:1008.3388. Bibcode:2011ApJ...742..116B. doi:10.1088/0004-637X/742/2/116. S2CID 119182075.
  5. ^ a b c d e Sun, Leilei; Gu, Shenghong; Wang, Xiaobin; Collier Cameron, Andrew; Cao, Dongtao; Wang, Yibo; Xiang, Yue; Hui, Ho-Keung; Kwok, Chi-Tai; Yeung, Bill; Ng, Eric; Grau Horta, Ferran (2017). "Refined System Parameters and TTV Study of Transiting Exoplanetary System HAT-P-20". The Astronomical Journal. 153 (1): 28. Bibcode:2017AJ....153...28S. doi:10.3847/1538-3881/153/1/28.
  6. ^ Ulmer-Moll, S.; Santos, N. C.; Figueira, P.; Brinchmann, J.; Faria, J. P. (2019). "Beyond the exoplanet mass-radius relation". Astronomy and Astrophysics. 630: A135. arXiv:1909.07392. Bibcode:2019A&A...630A.135U. doi:10.1051/0004-6361/201936049.
  7. ^ a b c d e f Esposito, M.; Covino, E.; Desidera, S.; Mancini, L.; Nascimbeni, V.; Zanmar Sanchez, R.; Biazzo, K.; Lanza, A. F.; Leto, G.; Southworth, J.; Bonomo, A. S.; Suárez Mascareño, A.; Boccato, C.; Cosentino, R.; Claudi, R. U.; Gratton, R.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Sozzetti, A.; Affer, L.; Anderson, D. R.; Andreuzzi, G.; Benatti, S.; Bignamini, A.; et al. (2017). "The GAPS Programme with HARPS-N at TNG. XIII. The orbital obliquity of three close-in massive planets hosted by dwarf K-type stars: WASP-43, HAT-P-20 and Qatar-2". Astronomy & Astrophysics. 601: A53. arXiv:1702.03136. Bibcode:2017A&A...601A..53E. doi:10.1051/0004-6361/201629720. S2CID 119341241.
  8. ^ Hamer, Jacob H.; Schlaufman, Kevin C. (2022). "Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities". The Astronomical Journal. 164 (1): 26. arXiv:2205.00040. Bibcode:2022AJ....164...26H. doi:10.3847/1538-3881/ac69ef.
  9. ^ HAT-P-20 -- High proper-motion Star
  10. ^ Salz, M.; Schneider, P. C.; Czesla, S.; Schmitt, J. H. M. M. (2015). "High-energy irradiation and mass loss rates of hot Jupiters in the solar neighborhood". Astronomy & Astrophysics. 576: A42. arXiv:1502.00576. Bibcode:2015A&A...576A..42S. doi:10.1051/0004-6361/201425243. S2CID 55139248.


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