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HAT-P-15: Difference between revisions

Coordinates: Sky map 04h 24m 59.5348s, +39° 27′ 38.3124″
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Revision as of 22:50, 19 March 2021

HAT-P-15
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 04h 24m 59.5348s[1]
Declination +39° 27′ 38.3124″[1]
Apparent magnitude (V) 12.41
Characteristics
Spectral type G5V
Astrometry
Radial velocity (Rv)31.21 km/s
Proper motion (μ) RA: 14.403 mas/yr
Dec.: -9.377 mas/yr
Parallax (π)5.1664 ± 0.0544 mas[1]
Distance631 ± 7 ly
(194 ± 2 pc)
Details[2]
Mass1.013±0.043 M☉
Radius1.080±0.039 R☉
Luminosity1.00±0.11 L☉
Surface gravity (log g)4.38±0.03 cgs
Temperature5684±25 K
Metallicity0.272±0.031
Rotational velocity (v sin i)2.0±0.5 km/s
Age6.8+2.5
−1.6 Gyr
Other designations
Gaia DR2 179498266829041664, TYC 2883-1687-1, GSC 02883-01687, 2MASS J04245952+3927382[1]
Database references
SIMBADdata

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.[2] The star has no noticeable starspot activity.[3]

The spectroscopic survey in 2015 have failed to find any stellar companions to it,[4] yet imaging survey have identified a possibly two companion red dwarf stars at projected separations 1210 and 1370 AU, respectively.[5]

The star was named Berehynia in December 2019 by the Ukrainian amateur astronomers.[6]

Planetary system

In 2010 a transiting hot superjovian planet b (named Tryzub in 2019[6]) was detected. It has an equilibrium temperature of 904±20 K.[7] The orbital simulation shown the planets inward of orbit of b would in-spiral and be destroyed within time-span of less than billion years.[8]

Size comparison of HAT-P-15 b and Jupiter
The HAT-P-15 planetary system[7]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 1.946±0.066 MJ 0.0964±0.0014 10.863502±0.000027 0.19±0.019 89.1±0.2° 1.072±0.043 RJ

References

  1. ^ a b c d HAT-P-15 -- Star
  2. ^ a b 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, doi:10.3847/1538-3881/ab4f79, S2CID 208527082{{citation}}: CS1 maint: unflagged free DOI (link)
  3. ^ Shkolnik, Evgenya L. (2013), "An Ultraviolet Investigation of Activity on Exoplanet Host Stars", The Astrophysical Journal, 766: 9, arXiv:1301.6192, doi:10.1088/0004-637X/766/1/9, S2CID 118415788
  4. ^ 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, arXiv:1510.08062, doi:10.1088/0004-637X/814/2/148, S2CID 11525988
  5. ^ 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
  6. ^ a b "Украина выбрала имена для звезды и экзопланеты". LIGA.net. Retrieved 2019-12-18.
  7. ^ a b 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, doi:10.1088/0004-637X/724/2/866, S2CID 119207125
  8. ^ 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


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