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KELT-6, also known as BD+31 2447, is a star in the constellation Coma Berenices. With an apparent magnitude of 10.34, it is impossible to see with the unaided eye, but can be seen with a powerful telescope. The star is located 791 light years away from the Solar System based on parallax, but is drifting away with a radial velocity of 1.62 km/s.

KELT-6
Observation data
Epoch J2000      Equinox J2000
Constellation Coma Berenices
Right ascension 13h 03m 55.65s[1]
Declination +30° 38′ 24.28″[1]
Apparent magnitude (V) 10.34±0.05[2]
Characteristics
Spectral type F8IV-V[2]
Astrometry
Radial velocity (Rv)1.62±0.27[1] km/s
Proper motion (μ) RA: −5.106±0.052 mas/yr[1]
Dec.: +15.640±0.046 mas/yr[1]
Parallax (π)4.1255 ± 0.0338 mas[1]
Distance791 ± 6 ly
(242 ± 2 pc)
Details
Mass1.13±0.06[3] M☉
Radius1.53±0.14[3] R☉
Luminosity3.25+0.94
−0.81[2] L☉
Surface gravity (log g)4.07±0.06[4] cgs
Temperature6,272±61[3] K
Metallicity [Fe/H]-0.28[4] dex
Rotational velocity (v sin i)4.53±0.26[5] km/s
Age4.9+0.7
−0.5[3] Gyr
Other designations
BD+31 2447, Gaia DR2 1464700950221781504
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

Properties


KELT-6 is an F-type star that is 13% more massive and 53% larger than the Sun. It radiates at 3.25 times the Sun's luminosity from its photosphere at an effective temperature of 6,727 K. KELT-6 has a projected rotational velocity of 4.53 km/s, and is slightly older than the Sun, with an age of 4.9 billion years. Unlike most hosts, the planet has a poor metallicity, with 52.5% the abundance of heavy metals compared to the Sun.


Planetary System


In 2013, a long period "hot Jupiter" was discovered orbiting the star using the transit method.[2] Another planet was discovered in 2015 using radial velocity (Doppler spectroscopy) method.[5]

The KELT-6 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 0.44±0.02[3] MJ 0.08±0.00[3] 7.85±0.00[3] 0.22±0.11[4] 88.81±0.85[4]° 1.18±0.11[3] RJ
c 3.71±0.21[5] MJ 2.39±0.11[5] 1,276+81
−67[5]		 0.21±0.04[5] — —

See also



References


  1. 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.
  2. Collins, Karen A.; Eastman, Jason D.; Beatty, Thomas G.; Siverd, Robert J.; Gaudi, B. Scott; Pepper, Joshua; Kielkopf, John F.; Johnson, John Asher; Howard, Andrew W.; Fischer, Debra A.; Manner, Mark (2014-02-01). "KELT-6b: A P ~ 7.9 Day Hot Saturn Transiting a Metal-poor Star with a Long-period Companion". The Astronomical Journal. 147: 39. arXiv:1308.2296. doi:10.1088/0004-6256/147/2/39. ISSN 0004-6256.
  3. Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A.; Lodato, G.; Marzari, F.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Covino, E.; Gratton, R.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Affer, L.; Biazzo, K.; Bignamini, A.; Esposito, M.; Giacobbe, P.; Hébrard, G.; Malavolta, L.; Maldonado, J.; Mancini, L.; Martinez Fiorenzano, A.; Masiero, S.; Nascimbeni, V.; Pedani, M.; Rainer, M.; Scandariato, G. (June 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 & Astrophysics. 602: A107. doi:10.1051/0004-6361/201629882.
  4. Stassun, Keivan G.; Collins, Karen A.; Gaudi, B. Scott (1 March 2017). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153: 136. arXiv:1609.04389. doi:10.3847/1538-3881/aa5df3. ISSN 0004-6256.
  5. Damasso, M.; Esposito, M.; Nascimbeni, V.; Desidera, S.; Bonomo, A. S.; Bieryla, A.; Malavolta, L.; Biazzo, K.; Sozzetti, A.; Covino, E.; Latham, D. W.; Gandolfi, D.; Rainer, M.; Petrovich, C.; Collins, K. A.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Gratton, R.; Lanza, A. F.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Di Fabrizio, L.; Giacobbe, P.; Gomez-Jimenez, M.; Murabito, S.; Molinaro, M.; Affer, L.; Barbieri, M.; Bedin, L. R.; Benatti, S.; Borsa, F.; Maldonado, J.; Mancini, L.; Scandariato, G.; Southworth, J.; Zanmar Sanchez, R. (1 September 2015). "The GAPS programme with HARPS-N at TNG. IX. The multi-planet system KELT-6: Detection of the planet KELT-6 c and measurement of the Rossiter-McLaughlin effect for KELT-6 b". Astronomy and Astrophysics. 581: L6. doi:10.1051/0004-6361/201526995. ISSN 0004-6361.

На других языках

- [en] KELT-6

[ru] KELT-6

KELT-6 — одиночная звезда в созвездии Волосы Вероники на расстоянии приблизительно 790 световых лет (около 242 парсеков) от Солнца. Видимая звёздная величина звезды — +10,42m[5]. Возраст звезды определён как около 4,9 млрд лет[6].


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