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] |
| Distance | 791 ± 6 ly (242 ± 2 pc) |
| Details | |
| Mass | 1.13±0.06[3] M☉ |
| Radius | 1.53±0.14[3] R☉ |
| Luminosity | 3.25+0.94 −0.81[2] L☉ |
| Surface gravity (log g) | 4.07±0.06[4] cgs |
| Temperature | 6,272±61[3] K |
| Metallicity [Fe/H] | -0.28[4] dex |
| Rotational velocity (v sin i) | 4.53±0.26[5] km/s |
| Age | 4.9+0.7 −0.5[3] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
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.
Properties
[edit]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 host stars of exoplanets, it has a poor metallicity, with 52.5% the abundance of heavy metals compared to the Sun.
Planetary system
[edit]In 2013, a long period "hot Jupiter" was discovered orbiting the star using the transit method.[2] Another planet was discovered in 2015 using the radial velocity (doppler spectroscopy) method.[5]
| 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
[edit]- List of most luminous stars
- List of most massive stars
- Lists of stars
- Lists of stars by constellation
References
[edit]- ^ a b c d e 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 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 (2): 39. arXiv:1308.2296. Bibcode:2014AJ....147...39C. doi:10.1088/0004-6256/147/2/39. ISSN 0004-6256. S2CID 15020416.
- ^ a b c d e f g h 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. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882.
- ^ a b c d 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 (3): 136. arXiv:1609.04389. Bibcode:2017AJ....153..136S. doi:10.3847/1538-3881/aa5df3. ISSN 0004-6256. S2CID 119219062.
- ^ a b c d e f 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. arXiv:1508.06520. Bibcode:2015A&A...581L...6D. doi:10.1051/0004-6361/201526995. ISSN 0004-6361.
