HAT-P-15

Last updated
HAT-P-15 / Berehynia
Observation data
Epoch J2000       Equinox J2000
Constellation Perseus
Right ascension 04h 24m 59.5350s [1]
Declination +39° 27′ 38.313″ [1]
Apparent magnitude  (V)12.41
Characteristics
Spectral type G5V
Variable type planetary transit [2]
Astrometry
Radial velocity (Rv)31.21 km/s
Proper motion (μ)RA: 14.233(21)  mas/yr [1]
Dec.: −9.407(15)  mas/yr [1]
Parallax (π)5.1856 ± 0.0166  mas [1]
Distance 629 ± 2  ly
(192.8 ± 0.6  pc)
Details [3]
Mass 1.013±0.043  M☉
Radius 1.080±0.039  R☉
Luminosity 1.00±0.11  L☉
Surface gravity (log g)4.38±0.03  cgs
Temperature 5684±25  K
Metallicity 0.272±0.031
Rotational velocity (v sin i)2.0±0.5 km/s
Age 6.8+2.5
−1.6  Gyr
Other designations
Berehynia, Gaia DR3  179498266829041664, TYC  2883-1687-1, GSC  02883-01687, 2MASS J04245952+3927382 [4]
Database references
SIMBAD data

HAT-P-15 is a G-type main-sequence star about 630 light-years away. The star is older than Sun yet has a concentration of heavy elements roughly 190% of solar abundance. [3] The star has no noticeable starspot activity. [5]

The spectroscopic survey in 2015 have failed to find any stellar companions to it, [6] yet imaging survey have identified a possibly two companion red dwarf stars at projected separations 1210 and 1370 AU, respectively. [7]

The star was named Berehynia in December 2019 by Ukrainian amateur astronomers. [8]

Planetary system

In 2010 a transiting hot superjovian planet b (named Tryzub in 2019 [8] ) was detected. It has an equilibrium temperature of 904±20 K. [2] An orbital simulation shows that any planets inward of the orbit of b would spiral inward and be destroyed within a time-span of less than a billion years. [9] The planetary orbit is well aligned with the equatorial plane of the star, misalignment equal to 13±6 degrees. [10]

Size comparison of HAT-P-15 b and Jupiter Exoplanet Comparison HAT-P-15 b.png
Size comparison of HAT-P-15 b and Jupiter
The HAT-P-15 planetary system [2]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b / Tryzub 1.946±0.066  MJ 0.0964±0.001410.863502±0.0000270.19±0.01989.1±0.2° 1.072±0.043  RJ

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References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  2. 1 2 3 Kovács, G.; Bakos, G. Á.; Hartman, J. D.; Torres, G.; Noyes, R. W.; Latham, D. W.; Howard, A. W.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Isaacson, H.; Sasselov, D. D.; Stefanik, R. P.; Esquerdo, G. A.; Fernandez, J. M.; Lázár, B. Béky J.; Papp, I.; Sári, P.; Sári, P. (2010), "HAT-P-15b: A 10.9-Day Extrasolar Planet Transiting a Solar-Type Star", The Astrophysical Journal, 724 (2): 866–877, arXiv: 1005.5300 , Bibcode:2010ApJ...724..866K, doi:10.1088/0004-637X/724/2/866, S2CID   119207125
  3. 1 2 Teske, Johanna K.; Thorngren, Daniel; Fortney, Jonathan J.; Hinkel, Natalie; Brewer, John M. (2019), "Do Metal-Rich Stars Make Metal-Rich Planets? New Insights on Giant Planet Formation from Host Star Abundances", The Astronomical Journal, 158 (6): 239, arXiv: 1912.00255 , Bibcode:2019AJ....158..239T, doi:10.3847/1538-3881/ab4f79, S2CID   208527082
  4. ↑ HAT-P-15 -- Star
  5. ↑ Shkolnik, Evgenya L. (2013), "An Ultraviolet Investigation of Activity on Exoplanet Host Stars", The Astrophysical Journal, 766 (1): 9, arXiv: 1301.6192 , Bibcode:2013ApJ...766....9S, doi:10.1088/0004-637X/766/1/9, S2CID   118415788
  6. ↑ Piskorz, Danielle; Knutson, Heather A.; Ngo, Henry; Muirhead, Philip S.; Batygin, Konstantin; Crepp, Justin R.; Hinkley, Sasha; Morton, Timothy D. (2015), "Friends of Hot Jupiters III: An Infrared Spectroscopic Search for Low-Mass Stellar Companions", The Astrophysical Journal, 814 (2): 148, arXiv: 1510.08062 , Bibcode:2015ApJ...814..148P, doi:10.1088/0004-637X/814/2/148, S2CID   11525988
  7. ↑ 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
  8. 1 2 "Украина выбрала имена для звезды и экзопланеты". LIGA.net. 18 December 2019. Retrieved 2019-12-18.
  9. ↑ Van Laerhoven, Christa; Greenberg, Richard (2014), "Small Inner Companions of Warm Jupiters: Lifetimes and Legacies", The Astrophysical Journal, 778 (2): 182, arXiv: 1401.7217 , doi:10.1088/0004-637X/778/2/182, S2CID   119297266
  10. ↑ Mancini, L.; et al. (2022), "The GAPS Programme at TNG", Astronomy & Astrophysics, 664: A162, arXiv: 2205.10549 , doi:10.1051/0004-6361/202243742, S2CID   248986121
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