KELT-6b

Last updated
KELT-6b
KELT-6b comparision.png
KELT-6b (white) compared to Jupiter
Discovery [1]
Discovered by Collins et al.
Discovery site KELTNorth
Discovery date2014
Transit
Orbital characteristics
0.0804±0.0014  AU [2]
Eccentricity 0.22±0.11 [3]
7.8457±0.0002  d [3]
Inclination 88.81° ±0.85° [3]
2,456,269.2+1.7
−2.5
  JD
[1]
308° +30°
−272°
[4]
Semi-amplitude 42.8±4.3  km/s [3]
Star KELT-6
Physical characteristics
Mean radius
1.30±0.09  RJ [3]
Mass 0.442±0.019  MJ [4]
Mean density
0.333+0.120
−0.079
  g/cm3
[2] (0.012+0.004
−0.002
  lb/cuin
)
Temperature 1313+59
−38
  K
[1]

    KELT-6b is an exoplanet orbiting the F-type subgiant KELT-6 approximately 791 light years away in the northern constellation Coma Berenices. It was discovered in 2013 using the transit method, and was announced in 2014.

    Contents

    Discovery

    In 2014, the planet's parameters were observed. The paper states that KELT-6 has just entered the subgiant phase, and is no longer on the main sequence. In 2015, an additional planet, c, was discovered using the radial velocity method. [4]

    Properties

    KELT-6b is a hot Saturn with 44.2% Jupiter's mass, but has been bloated to 1.3 times Jupiter's radius. It's density is half of Saturn's, and it has an equilibrium temperature of 1,313 K, but a hotter dayside temperature of 1,531 K. [5]

    Related Research Articles

    HAT-P-3, is a metal-rich K5 dwarf star located about 441 light-years away in the constellation Ursa Major. At a magnitude of about 11.5 it is not visible to the naked eye but is visible in a small to medium-sized amateur telescope. It is believed to be a relatively young star and has a slightly enhanced level of chromospheric activity.

    WASP-56 is a sun-like star of spectral type G6 in the constellation of Coma Berenices. It has an apparent magnitude of 11.48. Observations at the Calar Alto Observatory using the lucky imaging technique detected a candidate companion star located 3.4 arc seconds away, however it is not known if this is an actual binary companion or an optical double.

    HD 220773 is a 7th-magnitude star approximately 165 light years away in the constellation of Pegasus.

    Gliese 15 Ab, also commonly called Groombridge 34 Ab, is an extrasolar planet approximately 11 light-years away in the constellation of Andromeda. It is found in the night sky orbiting the star Gliese 15 A, which is at right ascension 00h 18m 22.89s and declination +44° 01′ 22.6″.

    Gliese 908 Star in the constellation Pisces

    Gliese 908 is a red dwarf star, located in constellation Pisces at 19.3 light-years from Earth. It is a BY Draconis variable star with a variable star designation of BR Piscium. Its apparent magnitude varies between magnitude 8.93 and magnitude 9.03 as a result of starspots and varying chromospheric activity.

    Ross 695, also known as Gliese 465, is a red dwarf star in the constellation Corvus. At apparent magnitude 11.27, it is much too faint to be seen with the unaided eye. A small star, it has around 23% the mass and radius of the Sun, but only 0.7% its luminosity. Investigation of its radial velocity failed to find any evidence of a planetary companion.

    HAT-P-20 is a K-type main-sequence star about 232 light-years away. The star has a strong starspot activity, and its equatorial plane is misaligned by 36+10
    −12
    ° with the planetary orbit. Although star with a giant planet on close orbit is expected to be spun-up by tidal forces, only weak indications of tidal spin-up were detected.

    Gliese 15 Ac Planet orbiting Gliese 15 A

    Gliese 15 Ac is an exoplanet orbiting the nearby red dwarf star Gliese 15 A, which is part of a binary star system located about 11.6 light-years from the Sun. The planet was first proposed in October 2017 using radial velocity data from the CARMENES spectrograph, combined with measurements from the HARPS and HIRES spectrographs, and its existence was confirmed in April 2018 using HARPS-N data. It has a minimum mass 36 times that of Earth and orbits at around 5.4 astronomical units with a period of 7,600 days, an orbit which may have been sculpted by interaction with the companion star, Gliese 15 B. As of 2020, Gliese 15 Ac is the longest-period sub-Jovian planet discovered by radial velocity.

    WASP-35 is a G-type main-sequence star about 660 light-years away. The star's age cannot be well constrained, but it is probably older than the Sun. WASP-35 is similar in concentration of heavy elements compared to the Sun.

    Qatar-2 is a K-type main-sequence star about 595 light-years away. The star is much older than Sun, and has a concentration of heavy elements similar to solar abundance. The star features a numerous and long-lived starspots, and belongs to a peculiar variety of inflated K-dwarfs with strong magnetic activity inhibiting internal convection.

    BD-11 4672 is a 9th magnitude orange dwarf star located 88.7 light-years away in the constellation of Scutum. This star was recognised as a high proper motion star by Max Wolf in 1924. It is a single star, and is the host to two known extrasolar planets.

    BD+00 316, also known as WASP-71 since 2019, is an F-class main sequence star about 1200 light-years away. The star is younger than the Sun at approximately 3.6 billion years, yet is already close to leaving the main sequence. BD+00 316 is enriched in heavy elements, having 140% of the solar abundance of iron.

    WASP-59 is a K-type main-sequence star about 379 light-years away. The star's age is essentially unconstrained by observations. WASP-59 is slightly depleted in heavy elements, having 70% of the solar abundance of iron. The star produces extremely low levels of ultraviolet light, indicating an absence of flare activity.

    WASP-54, also known as BD+00 3088, is a binary star system about 825 light-years away. The primary, WASP-54A, is a F-type main-sequence star, accompanied by the red dwarf WASP-54B on a wide orbit. WASP-54 is depleted in heavy elements, having 55% of the solar abundance of iron. The age of WASP-54 is slightly older than the Sun's at 6.9+1.0
    −1.9
    billion years.

    WASP-42 is a K-type main-sequence star. Its surface temperature is 5315±79 K. WASP-42 is similar to the Sun in concentration of heavy elements, with metallicity ([Fe/H]) of 0.05±0.13, and is much older than the Sun at 11.3+1.5
    −4.8
    billion years. The star does exhibit starspot activity as is typical for its spectral class.

    WASP-41 is a G-type main-sequence star. Its surface temperature is 5450±150 K. WASP-41 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of −0.080±0.090, but is much younger at an age of 2.289±0.077 billion years. The star does exhibit strong starspot activity, with spots covering 3% of the stellar surface.

    HAT-P-41 is a binary star system. Its primary is a F-type main-sequence star. Its surface temperature is 6390±100 K. compared to the Sun, HAT-P-41 is enriched in heavy elements, with a metallicity Fe/H index of 0.21±0.10, but is much younger at an age of 2.2±0.4 billion years.

    WASP-88 is a F-type main-sequence star. Its surface temperature is 6450±61 K. WASP-88 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.03±0.04, and is younger at an age of 3.0±1.3 billion years.

    BD+02 2056, also known as WASP-84 is a G-type main-sequence star. Its surface temperature is 5350±31 K, and is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.05±0.02. It is rich in carbon and depleted of oxygen. BD+02 2056's age is probably older than the Sun at 8.5+4.1
    −5.5
    billion years. The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.

    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.

    References

    1. 1 2 3 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; Bieryla, Allyson; Latham, David W.; Fulton, Benjamin J.; Gregorio, Joao; Buchhave, Lars A.; Jensen, Eric L. N.; Stassun, Keivan G.; Penev, Kaloyan; Crepp, Justin R.; Hinkley, Sasha; Street, Rachel A.; Cargile, Phillip; Mack, Claude E.; Oberst, Thomas E.; Avril, Ryan L.; Mellon, Samuel N.; McLeod, Kim K.; Penny, Matthew T.; Stefanik, Robert P.; Berlind, Perry; Calkins, Michael L.; Mao, Qingqing; Richert, Alexander J. W.; DePoy, Darren L.; Esquerdo, Gilbert A.; Gould, Andrew; Marshall, Jennifer L.; Oelkers, Ryan J.; Pogge, Richard W.; Trueblood, Mark; Trueblood, Patricia (1 February 2014). "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.
    2. 1 2 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 and Astrophysics. 602: A107. arXiv: 1704.00373 . Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882. ISSN   0004-6361. S2CID   118923163.
    3. 1 2 3 4 5 Stassun, Keivan G.; Collins, Karen A.; Gaudi, B. Scott (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.
    4. 1 2 3 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. S2CID   119114846.
    5. "KELT-6 b". www.exoplanetkyoto.org. Retrieved 2021-08-13.