| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Andromeda[1] |
| Right ascension | 23h 39m 05.8103s[2] |
| Declination | +42° 27′ 57.505″[2] |
| Apparent magnitude (V) | +10.47[3] |
| Characteristics | |
| Spectral type | F8V[4] |
| B−V color index | 0.41[3] |
| Variable type | planetary transit[5] |
| Astrometry | |
| Radial velocity (Rv) | −22.13(44)[6] km/s |
| Proper motion (μ) | RA: −20.202(18) mas/yr[2] Dec.: 2.996(18) mas/yr[2] |
| Parallax (π) | 3.6459 ± 0.0221 mas[2] |
| Distance | 895 ± 5 ly (274 ± 2 pc) |
| Absolute magnitude (MV) | +3.36(16)[5] |
| Details | |
| Mass | 1.29 ± 0.06[7] M☉ |
| Radius | 1.46 ± 0.06[7] R☉ |
| Luminosity | 3.57+0.52 −0.43[5] L☉ |
| Surface gravity (log g) | 4.22 ± 0.03[8] cgs |
| Temperature | 6,570 ± 80[7] K |
| Metallicity [Fe/H] | –0.13 ± 0.08[7] dex |
| Rotational velocity (v sin i) | 8.7 ± 1.0[7] km/s |
| Age | 2.3+0.5 −0.7[7] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Extrasolar Planets Encyclopaedia | data |
HAT-P-6 also named Sterrennacht[10] is a star in the constellation Andromeda, located approximately 895 light years or 274 parsecs away from the Earth. It is an F-type star, implying that it is hotter and more massive than the 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.[11]
The name Sterrennacht (Starry Night) was selected in the NameExoWorlds held by the IAU after a painting by Van Gogh.[10]
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Transcription
Planetary system
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.[12]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b / Nachtwacht | 1.106+0.039 −0.040 MJ |
0.05239+0.00080 −0.00082 |
3.852985±0.000005 | <0.044 | 166±10[12]° | 1.330±0.061 RJ |
See also
References
- ^ 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
- ^ a b c d 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.
- ^ 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.
- ^ 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. S2CID 21090559.
- ^ a b c d e f 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. S2CID 2301387.
- ^ 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.
- ^ 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. S2CID 118923163.
- ^ 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. S2CID 16580774.
- ^ "HAT-P-6". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-02-26.
- ^ a b "Approved names". NameExoworlds. Retrieved 2020-01-02.
- ^ 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. S2CID 119117620.
- ^ a b Hébrard, Guillaume; Ehrenreich, David; Bouchy, François; Delfosse, Xavier; Moutou, Claire; Arnold, Luc; Boisse, Isabelle; Bonfils, Xavier; Díaz, Rodrigo F.; Eggenberger, Anne; Forveille, Thierry; Lagrange, Anne-Marie; Lovis, Christophe; Pepe, Francesco; Perrier, Christian; Queloz, Didier; Santerne, Alexandre; Santos, Nuno C.; Ségransan, Damien; Udry, Stéphane; Vidal-Madjar, Alfred (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. S2CID 56130884.
External links
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This page was last edited on 24 August 2023, at 12:26