HAT-P-28

HAT-P-28
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 00h 52m 00.1876s[1]
Declination +34° 43′ 42.205″[1]
Apparent magnitude (V) 13.03[2]
Characteristics
Evolutionary stage main-sequence star
Spectral type G
Astrometry
Radial velocity (Rv)48.06[3] km/s
Proper motion (μ) RA: 25.615(14) mas/yr[1]
Dec.: 2.712(11) mas/yr[1]
Parallax (π)2.4728 ± 0.0156 mas[1]
Distance1,319 ± 8 ly
(404 ± 3 pc)
Orbit[4]
PrimaryHAT-P-28
CompanionHAT-P-28 B
Semi-major axis (a)0.994±0.002"
(404 AU)
Details[5]
Mass1.02±0.05 M☉
Radius1.10+0.09
−0.07 R☉
Luminosity1.13+0.23
−0.16[2] L☉
Surface gravity (log g)4.36±0.06[2] cgs
Temperature5680±90[2] K
Metallicity [Fe/H]0.12±0.08[2] dex
Rotational velocity (v sin i)0.2+0.5
−0.2[2] km/s
Age6.1+2.6
−1.9[2] Gyr
Other designations
Gaia DR2 363702817083391232, GSC 02284-00503, 2MASS J00520018+3443422[3]
Database references
SIMBADdata

HAT-P-28 is the primary of a binary star system about 1320 light-years away. It is a G-type main-sequence star. The star's age is older than the Sun's at 6.1+2.6
−1.9 billion years.[2] HAT-P-28 is slightly enriched in heavy elements, having a 130% concentration of iron compared to the Sun. Since 2014, the binary star system is suspected to be surrounded by a debris disk with a 6.1″(2500 AU) radius.[6]

The red dwarf stellar companion was detected in 2015 at a projected separation of 0.972″[7] and confirmed in 2016 to be either bound or comoving.[4]

  1. ^ a b c d Cite error: The named reference Gaia DR3 was invoked but never defined (see the help page).
  2. ^ a b c d e f g h Cite error: The named reference Buchhave2011 was invoked but never defined (see the help page).
  3. ^ a b Cite error: The named reference simbad was invoked but never defined (see the help page).
  4. ^ a b 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 (1): 8, arXiv:1606.07102, Bibcode:2016ApJ...827....8N, doi:10.3847/0004-637X/827/1/8, S2CID 41083068
  5. ^ 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, Bibcode:2018AJ....155..165P, doi:10.3847/1538-3881/aaaf71, PMC 6510550, PMID 31080254, S2CID 64370118
  6. ^ Merín, Bruno; Ardila, David R.; Ribas, Álvaro; Bouy, Hervé; Bryden, Geoffrey; Stapelfeldt, Karl; Padgett, Deborah (2014), "Herschel/PACS photometry of transiting-planet host stars with candidate warm debris disks", Astronomy & Astrophysics, 569: A89, arXiv:1409.0572, Bibcode:2014A&A...569A..89M, doi:10.1051/0004-6361/201322956, S2CID 10038821
  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