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Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Andromeda[1]
Right ascension  23h 39m 05.8101s[2]
Declination +42° 27′ 57.5034″[2]
Apparent magnitude (V) +10.47[3]
Spectral type F8V[4]
B−V color index 0.41[3]
Variable type planetary transit
Radial velocity (Rv)−22.13±0.44[2] km/s
Proper motion (μ) RA: −20.075±0.074[2] mas/yr
Dec.: 3.123±0.049[2] mas/yr
Parallax (π)3.6036 ± 0.0470[2] mas
Distance910 ± 10 ly
(278 ± 4 pc)
Absolute magnitude (MV)+3.36±0.16[5]
Mass1.29 ± 0.06[6] M
Radius1.46 ± 0.06[6] R
[5] L
Surface gravity (log g)4.22 ± 0.03[7] cgs
Temperature6,570 ± 80[6] K
Metallicity [Fe/H]–0.13 ± 0.08[6] dex
Rotational velocity (v sin i)8.7 ± 1.0[6] km/s
[6] Gyr
Other designations
GSC 03239-00992, 2MASS J23390581+4227575, TYC 3239-992-1
Database references
Extrasolar Planets

HAT-P-6 also named Sterrennacht[8] is a star in the constellation Andromeda, located approximately 910 light years or 280 parsecs away from the Earth. It is an F-type star, implying that it is hotter and more massive than our Sun. The apparent magnitude of the star is +10.54, which means that it can only be visible through the telescope. The absolute magnitude of +3.36 is brighter than the Sun's +4.83, meaning that the star itself is brighter than the Sun.[5] A search for a binary companion star using adaptive optics at the MMT Observatory turned out negative.[9]

The name Sterrennacht (Starry Night) was selected in the NameExoWorlds held by the IAU by the Netherlands is a world-famous painting by Dutch grand master Van Gogh.[8]

Planetary system[edit]

The companion planet HAT-P-6b is a transiting planet discovered on October 15, 2007 by the HATNet Project. The planet's true mass is slightly more than Jupiter at only 5.7%, but the radius is 33% greater, making the planet's density of 0.45 g/cm3. Its large size compared to mass comes from the great amount of heat received from the nearby star that expands the planet's atmosphere, categorizing as "hot Jupiter". The orbital period is 3.852985 days and the distance from its star is 0.05235 AU.[5] The inclination of the orbit with respect to the stellar rotation axis is roughly 166º.[10]

The HAT-P-6 planetary system[5][6]
(in order from star)
Mass Semimajor axis
Orbital period
Eccentricity Inclination Radius
b 1.106+0.039
3.852985±0.000005 <0.044 166±10[10]° 1.330±0.061 RJ

See also[edit]


  1. ^ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi:10.1086/132034.Vizier query form
  2. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  3. ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H.
  4. ^ Faedi, F.; Staley, T.; Gómez Maqueo Chew, Y.; Pollacco, D.; Dhital, S.; Barros, S. C. C.; Skillen, I.; Hebb, L.; MacKay, C.; Watson, C. A. (2013). "Lucky imaging of transiting planet host stars with LuckyCam". Monthly Notices of the Royal Astronomical Society. 433 (3): 2097. arXiv:1305.3795. Bibcode:2013MNRAS.433.2097F. doi:10.1093/mnras/stt885.
  5. ^ a b c d e Noyes, R. W.; et al. (2008). "HAT-P-6b: A Hot Jupiter Transiting a Bright F Star". The Astrophysical Journal Letters. 673 (1): L79–L82. arXiv:0710.2894. Bibcode:2008ApJ...673L..79N. doi:10.1086/527358.
  6. ^ a b c d e f g Bonomo, A. S.; et al. (2017). "The GAPS Programme with HARPS-N at TNG . XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy and Astrophysics. 602. A107. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882.
  7. ^ Torres, Guillermo; et al. (2012). "Improved Spectroscopic Parameters for Transiting Planet Hosts". The Astrophysical Journal. 757 (2). 161. arXiv:1208.1268. Bibcode:2012ApJ...757..161T. doi:10.1088/0004-637X/757/2/161.
  8. ^ a b "Approved names". NameExoworlds. Retrieved 2020-01-02.
  9. ^ Adams, E. R.; et al. (2013). "Adaptive Optics Images. II. 12 Kepler Objects of Interest and 15 Confirmed Transiting Planets". The Astronomical Journal. 146 (1). 9. arXiv:1305.6548. Bibcode:2013AJ....146....9A. doi:10.1088/0004-6256/146/1/9.
  10. ^ a b Hébrard, G.; Ehrenreich, D.; Bouchy, F.; Delfosse, X.; Moutou, C.; Arnold, L.; Boisse, I.; Bonfils, X.; Díaz, R. F.; Eggenberger, A.; Forveille, T.; Lagrange, A. -M.; Lovis, C.; Pepe, F.; Perrier, C.; Queloz, D.; Santerne, A.; Santos, N. C.; Ségransan, D.; Udry, S.; Vidal-Madjar, A.; Smareglia, R.; Affer, L.; Biazzo, K.; Bignamini, A.; Esposito, M.; Giacobbe, P.; Hébrard, G.; Malavolta, L.; et al. (2011). "The retrograde orbit of the HAT-P-6b exoplanet". Astronomy and Astrophysics. 527: L11. arXiv:1101.5009. Bibcode:2011A&A...527L..11H. doi:10.1051/0004-6361/201016331.

External links[edit]

Coordinates: Sky map 23h 39m 05.8061s, +42° 27′ 57.513″